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J.At.Mol.Sci.doi:10.4208/jams.032510.042010a Vol.1,No.3,pp.201-214 August2010Theoretical Raman and IR spectra of tegafur andcomparison of molecular electrostatic potentialsurfaces,polarizability and hyerpolarizability oftegafur with5-fluoro-uracil by density functionaltheoryOnkar Prasad∗,Leena Sinha,and Naveen KumarDepartment of Physics,University of Lucknow,Lucknow,Pin Code-226007,IndiaReceived25March2010;Accepted(in revised version)20April2010Published Online28June2010Abstract.The5-fluoro-1-(tetrahydrofuran-2-yl)pyrimidine-2,4(1H,3H)-dione,also knownas tegafur,is an important component of Tegafur-uracil(UFUR),a chemotherapy drugused in the treatment of cancer.The equilibrium geometries of”Tegafur”and5-fluoro-uracil(5-FU)have been determined and analyzed at DFT level employing the basis set6-311+G(d,p).The molecular electrostatic potential surface which displays the activitycentres of a molecule,has been used along with frontier orbital energy gap,electricmoments,first static hyperpolarizability,to interpret the better selectivity of prodrugtegafur over the drug5-FU.The harmonic frequencies of prodrug tegafur have alsobeen calculated to understand its complete vibrational dynamics.In general,a goodagreement between experimental and calculated normal modes of vibrations has beenobserved.PACS:31.15.E-,31.15.ap,33.20.TpKey words:prodrug,polarizability,hyperpolarizability,frontier orbital energy gap,molecular electrostatic potential surface.1IntroductionThe use of a prodrug strategy increases the selectivity and thus results in improved bioavailability of the drug for its intended target.In case of chemotherapy treatments,the reduction of adverse effects is always of paramount importance.The prodrug whichis used to target the cancer cell has a low cytotoxicity,prior to its activation into cytotoxic form in the cell and hence there is a markedly lower chance of it”attacking”the healthy∗Corresponding author.Email address:prasad onkar@lkouniv.ac.in(O.Prasad)/jams201c 2010Global-Science Press202O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214 non-cancerous cells and thus reducing the side-effects associated with the chemothera-peutic agents.Tegafur,a prodrug and chemically known as5-fluoro-1-(tetrahydrofuran-2-yl)pyrimidine-2,4(1H,3H)-dione,is an important component of’Tegafur-uracil’(UFUR), a chemotherapy drug used in the treatment of cancer,primarily bowel cancer.UFUR is a first generation Dihydro-Pyrimidine-Dehydrogenase(DPD)inhibitory Flouropyrimidine drug.UFUR is an oral agent which combines uracil,a competitive inhibitor of DPD,with the5-FU prodrug tegafur in a4:1molar ratio.Excess uracil competes with5-FU for DPD, thus inhibiting5-FU catabolism.The tegafur is taken up by the cancer cells and breaks down into5-FU,a substance that kills tumor cells.The uracil causes higher amounts of 5-FU to stay inside the cells and kill them[1–4].The present communication deals with the investigation of the structural,electronic and vibrational properties of tegafur due to its biological and medical importance infield of cancer treatment.The structure and harmonic frequencies have been determined and analyzed at DFT level employing the basis set6-311+G(d,p).The optimized geometry of tegafur and5-FU and their molecular properties such as equilibrium energy,frontier orbital energy gap,molecular electrostatic potential energy map,dipole moment,polar-izability,first static hyperpolarizability have also been used to understand the properties and activity of the drug and prodrug.The normal mode analysis has also been carried out for better understanding of the vibrational dynamics of the molecule under investi-gation.2Computational detailsGeometry optimization is one of the most important steps in the theoretical calculations. The X-ray diffraction data of the tegafur monohydrate and the drug5-FU,obtained from Cambridge Crystallographic Data Center(CCDC)were used to generate the initial co-ordinates of the prodrug tegafur and drug5-FU to optimize the structures.The Becke’s three parameter hybrid exchange functionals[5]with Lee-Yang-Parr correlation func-tionals(B3LYP)[6,7]of the density functional theory[8]and6-311+G(d,p)basis set were chosen.All the calculations were performed using the Gaussian03program[9].TheFigure1:Optimized structure of Tegafur and5-fluoro-uracil at B3LYP/6-311+G(d,p).O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214203Figure2:Experimental and theoretical Raman spectra of Tegafur.model molecular structure of prodrug tegafur and drug5-FU are given in the Fig.1.Pos-itive values of all the calculated vibrational wave numbers confirmed the geometry to be located on true local minima on the potential energy surface.As the DFT hybrid B3LYP functional tends to overestimate the fundamental normal modes of vibration,a scaling factor of0.9679has been applied and a good agreement of calculated modes with ex-perimental ones has been obtained[10,11].The vibrational frequency assignments have been carried out by combining the results of the Gaussview3.07program[12],symmetry considerations and the VEDA4program[13].The Raman intensities were calculated from the Raman activities(Si)obtained with the Gaussian03program,using the following relationship derived from the intensity theory of Raman scattering[14,15]I i=f(v0−v i)4S iv i{1−exp(−hc v i/kT)},(1)where v0being the exciting wave number in cm−1,v i the vibrational wave number of i th normal mode,h,c and k universal constants and f is a suitably chosen common nor-malization factor for all peak intensities.Raman spectra has been calculated according to the spectral database for organic compounds(SDBS)literature,using4880˚A as excit-ing wavelength of laser source with200mW power[16].The calculated Raman and IR spectra have been plotted using the pure Lorentzian band shape with a band width of FWHM of3cm−1and are shown in Fig.2and Fig.3,respectively.204O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214Figure3:Experimental and theoretical IR spectra of Tegafur.The density functional theory has also been used to calculate the dipole moment, mean polarizability<α>and the totalfirst static hyperpolarizabilityβ[17,18]are given as for both the molecules in terms of x,y,z components and are given by following equationsµ=(µ2x+µ2y+µ2z)1/2(2)<α>=13αxx+αyy+αzz,(3)βTOTAL=β2x+β2y+β2z1/2=(βxxx+βxyy+βxzz)2+(βyyy+βyxx+βyzz)2+(βzzz+βzxx+βzyy)21/2.(4)Theβcomponents of Gaussian output are reported in atomic units and therefore the calculated values are converted into e.s.u.units(1a.u.=8.3693×10−33e.s.u.).O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214205 3Results and discussion3.1Geometric structureThe electronic structure of prodrug tegafur and the drug5-FU have been investigated, in order to assess the effect of introduction offive-membered ring having an electron withdrawing carbonyl group to the drug5-FU for better selectivity of target cancer cells. The optimized molecular structures with the numbering scheme of the atoms are shown in Fig. 1.The ground state optimized parameters are reported in Table1.Thefive-membered ring in case of tegafur adopts an envelope conformation,with the C(14)atom, acting as theflap atom,deviating from the plane through the remaining four carbon atoms.The C-C and C-H bond lengths offive-membered rings lie in the range1.518˚A ∼1.556˚A and1.091˚A∼1.096˚A respectively.The endocyclic angles offive-membered ring lie between103.50to108.00whereas there is a sharp rise in the endohedral angle values(129.1◦)at N(6)atom and sharp fall in the angle values(111.3◦)at C(8)atom in the six-membered hetrocyclic ring.The C(7)=O(2)/C(8)=O(3)/C(12)=O(4)bond lengths are equal to1.217/1.211/1.202˚A and are found to be close to the standard C=O bond length(1.220˚A).These calculated bond length,bond angles are in full agreement with those reported in[19,20].The skeleton of tegafur molecule is non-planar while the5-FU skeleton is planar.The optimized parameters agree well with the work reported by Teobald et al.[21].The angle between the hetrocyclic six-membered ring plane andfive-membered ring plane represented byζ(N(5)-C(11)-C(15)-C(12))is calculated at126.1◦.It is seen that most of the bond distances are similar in tegafur and5-FU molecules,al-though there are differences in molecular formula.In the six-membered ring all the C-C and C-N bond distances are in the range1.344∼1.457˚A and1.382∼1.463˚A.Accord-ing to our calculations all the carbonyl oxygen atoms carry net negative charges.The significance of this is further discussed in terms of its activity in the next section.Table1:Parameters corresponding to optimized geometry at DFT/B3LYP level of theory for Tegafur and5-FUParameters Tegafur5-FUGround state energy(in Hartree)-783.639204-514.200506Frontier orbital energy gap(in Hartree)0.185850.19593Dipole moment(in Debye) 6.43 4.213.2Electronic propertiesThe frontier orbitals,HOMO and LUMO determine the way a molecule interacts with other species.The frontier orbital gap helps characterize the chemical reactivity and ki-netic stability of the molecule.A molecule with a small frontier orbital gap is more po-larizable and is generally associated with a high chemical reactivity,low kinetic stability206O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214 and is also termed as soft molecule[22].The frontier orbital gap in case of prodrug tega-fur is found to be0.27429eV lower than the5-FU molecule.The HOMO is the orbital that primarily acts as an electron donor and the LUMO is the orbital that largely acts as the electron acceptor.The3D plots of the frontier orbitals HOMO and LUMO,electron density(ED)and the molecular electrostatic potential map(MESP)for both the molecules are shown in Fig.4and Fig.5.It can be seen from thefigures that,the HOMO is almost distributed uniformly in case of prodrug except the nitrogen atom between the two car-bonyl groups but in case of5-FU the HOMO is spread over the entire molecule.Homo’s of both the molecules show considerable sigma bond character.The LUMO in case of tegafur is found to be shifted mainly towards hetrocyclic ring and the carbonyl group offive-membered ring and shows more antibonding character as compared to LUMO of 5-FU in which the spread of LUMO is over the entire molecule.The nodes in HOMO’s and LUMO’s are placed almost symmetrically.The ED plots for both molecules show a uniform distribution.The molecular electrostatic potential surface MESP which is a plot of electrostatic potential mapped onto the iso-electron density surface,simultaneously displays molecular shape,size and electrostatic potential values and has been plotted for both the molecules.Molecular electrostatic potential(MESP)mapping is very use-ful in the investigation of the molecular structure with its physiochemical property rela-tionships[22–27].The MESP map in case of tegafur clearly suggests that each carbonyl oxygen atom of thefive and six-membered rings represent the most negative potential region(dark red)but thefluorine atom seems to exert comparatively small negative po-tential as compared to oxygen atoms.The hydrogen atoms attached to the six andfive-membered ring bear the maximum brunt of positive charge(blue region).The MESP of tegafur shows clearly the three major electrophyllic active centres characterized by red colour,whereas the MESP of the5-FU reveals two major electrophyllic active centres,the fluorine atom seems to exert almost neutral electric potential.The values of the extreme potentials on the colour scale for plotting MESP maps of both molecules have been taken same for the sake of comparison and drawing the conclusions.The predominance of green region in the MESP surfaces corresponds to a potential halfway between the two extremes red and dark blue colour.From a closer inspection of various plots given in Fig. 4and Fig.5and the electronic properties listed in Table1,one can easily conclude how the substitution of the hydrogen atom by thefive-membered ring containing an electron withdrawing carbonyl group modifies the properties of the drug5-FU.3.3Electric momentsThe dipole moment in a molecule is an important property that is mainly used to study the intermolecular interactions involving the non bonded type dipole-dipole interactions, because higher the dipole moment,stronger will be the intermolecular interactions.The calculated value of dipole moment in case of tegafur is found to be quite higher than the drug5-FU molecule and is attributed due to the presence of an extra highly electron withdrawing carbonyl group.The calculated dipole moment for both the molecules areO.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214207Table2:Polarizability data/a.u.for Tegafur at DFT/B3LYP level of theoryPolarizability TegafurαXX173.315αXY-2.494αYY111.365αXZ-4.149αYZ0.399αZZ92.930<α>125.870Table3:Allβcomponents andβTotal for Tegafur calculated at DFT/B3LYP level of theoryPolarizability TegafurβXXX-54.9411βXXY-57.5539βXYY-13.4605βYYY95.0387βXXZ31.8370βXYZ9.2943βYYZ-22.0880βXZZ57.6657βYZZ-21.7419βZZZ-37.3655βTotal(e.s.u.)0.2808×10−30also given in Table1.The lower frontier orbital energy gap and very high dipole moment for the tegafur are manifested in its high reactivity and consequently higher selectivity for the target carcinogenic/tumor cells as compared to5-FU(refer to Table1).According to the present calculations,the mean polarizability of tegafur(125.870/ a.u.,refer to Table2)is found significantly higher than5-FU(66.751/a.u.calculated at the same level of theory as well as same basis set).This is related very well to the smaller frontier orbital gaps of tegafur as compared to5-FU[22].The different components of polarizability are reported in the Table2.Thefirst static hyperpolarizabilityβcalculated value is found to be appreciably lowered in case of tegafur(0.2808x10−30e.s.u.,refer to Table3)as compared to5-FU(0.6218x10−30e.s.u.calculated at B3LYP/6-311+G(d,p)). Table3presents the different components of static hyperpolarizability.In addition,βval-ues do not seem to follow the same trend asαdoes,with the frontier orbital energy gaps. This behavior could be explained by a poor communication between the two frontier or-bitals of tegafur.Although the HOMO is almost distributed uniformly in case of tegafur208O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214Figure4:Plots of Homo,Lumo and the energy gaps in Tegafur and5-FU.Figure5:Total Density and MESP of Tegafur and5-FU.but the LUMO is found to be shrunk and shifted mainly towards hetrocyclic ring and the carbonyl group offive-membered ring and shows more antibonding character than the LUMO of5-FU.It may thus be concluded that the higher”selectivity”of the prodrug tegafur as compared to the drug5-FU may be attributed due to the higher dipole mo-ment and lower values of frontier energy band gap coupled with the lowerfirst static hyperpolarizability.3.4Vibrational spectral analysisAs the molecule has no symmetry,all the fundamental modes are Raman and IR active. The66fundamental modes of vibrations of tegafur are distributed among the functional and thefinger print region.The experimental and computed vibrational wave num-O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214209 bers,their IR and Raman intensities and the detailed description of each normal mode of vibration of the prodrug tegafur,carried out in terms of their contribution to the total potential energy are given in Table4.The calculated Raman and IR spectra of prodrugTable4:Theoretical and experimental a wave numbers(in cm−1)of TegafurExp a Exp a Calc.Calc.Calc.Calc.Assignment of dominantIR Raman(Unscaled(Scaled IR Raman modes in order of Wave no.Wave no.Wave no.Wave no.Intensity Intensity decreasing potentialin cm−1in cm−1in cm−1)in cm−1)energy distribution(PED)3426-3592347779.8317.38υ(N-H)(100)3076310032193115 3.0919.49υ(C-H)R(99)3033-3117301714.2012.97υas methylene(C-H)(82)30333004310730079.8732.29υas methylene(C-H)(90)-29763097299818.5945.83υas methylene(C-H)(80)--3065296720.6530.88υs methylene(C-H)(96)--305029527.8416.11υ(C-H)pr(98)--3044294610.2419.02υs methylene(C-H)(91)2911-3033293624.9745.77υs methylene(C-H)(84)1721-183********.637.65υ(C12=O)pr(90)1693172317821725461.2581.78υ(C8=O)R(72)1668170717661709871.67 3.93υ(C7=O)R(66)165816611701164776.0842.39υ(C9-C10)(66)+β(H17-C10-C9)(11)14711473151114628.71 2.05sc CH2(93)14661469149314457.829.82sc CH2(87)140014381467142042.97 1.93υ(N5-C)10)(23)+β(N5-C10-C9)(13) +υ(N6-C8)(11)+β(N5-C11-H18)(10)140014031450140320.857.15sc(CH2)(88)13621367141913738.94 3.78β(H16-N6-C7)(52)+υ(C=O)R(20) +β(H17-C10-N5)(11)135613401393134971.90 4.40β(H18-C11-N5)(35) +β(H16-N6-C7)(13)1339-138********.7460.20β(H17-C10-C9)(21)+υ(C9-C10)(14) +υ(N5-C10)(13)+υ(N6-C7)(12)--1343130010.26 1.21methylene(C14)wag(62)+methylene(C15)twisting(13)--1337129414.487.82methylene(C15)wag(56)+methylene(C14)twisting(16)1264126113071266 4.21 1.73methylene(C13)wag(56)+methylene(C14),(C15)twisting(16)1264-12991257 1.958.16Methylene twisting(60)1231-12671225199.09 4.95β(H17-C10-N5)(23)+methylene(C13)twisting(15) +υ(N5-C10)(10)1187-1244120485.739.03Ring deformation1179119912281189 4.29 1.65Methylene twisting(40) +(C11-H18)wag(35)--1193115522.238.09methylene(C13)wag(10) +β(H17-C10-C9)(10)210O.Prasad,L.Sinha,and N.Kumar/J.At.Mol.Sci.1(2010)201-214(continued)Exp a Exp a Calc.Calc.Calc.Calc.Assignment of dominantIR Raman(Unscaled(Scaled IR Raman modes in order of Wave no.Wave no.Wave no.Wave no.Intensity Intensity decreasing potentialin cm−1in cm−1in cm−1)in cm−1)energy distribution(PED)1115-11681131134.60 4.73β(H23-C15-C11)(21) +β(H22-C13-C14)(18)β(H16-N6-C7)(17)1115-11571120 5.9920.48υ(N6-C7)(30)+υ(N5-C10)(16) +methylene twisting(14)1065104510621028 3.60 4.26υ(C-C)pr(28)+β(H18-C11-C12)(13) +methylene twisting(11)1087-1126109020.609.14υ(C-C)pr(35)+β(C12-C13-C14)(12) --10139808.56 6.79υ(C-C)pr(54)+methylene wag(25)941942965934 2.79 1.53υ(C-C)pr(20)+β(H18-C11-C15)(17) +methylene twisting(10)9139219268970.27 6.28methylene rocking(33) +υ(C-C)pr(11)--916886 4.1310.06υ(C-C)pr(59)867-896868 2.20 5.99C-H out of plane Ring wag(79)840-8868570.48 4.53β(H16-N6-C7)(20)+β(H17-C10-C9)(13)+methylene(C13)rocking(13) +methylene(C14)twisting(11)--82780011.31 6.48methylene rocking(69)77378281578950.9325.00β(C10-N5-C7)(27)+β(C9-C10-N5)(16) +υ(F-C)(11)749-760736 5.940.73βout(O-C-N)(78)--75473052.72 2.02βout(O-C-N)(77)+(N-H)wag(10) --746722 5.537.78Ring Breathing mode(51)687704728705 1.7330.18methylene rocking(39) +β(O2-C7-N6)(18)-6466686479.5512.38β(O-C-N)(45)+β(F-C-C)(11) -64665863742.75 2.90(N-H)wag(90)608-6266069.55 2.91β(C-C-C)Pr(18)+β(O-C-C)Pr(18) +(N-H)wag(12)--58256320.4212.86βout(C-C-C)Pr(17)+β(C8-N6-C7)(12) +β(C9-C10-N5)(10)542-550532 2.497.84βout(C-C-C)Pr(31)+β(O-C-C)Pr(15)48249051850110.7119.07β(O-C-C)Pr(32)+Pr torsional mode(12) +Ring Tors.mode(12)430-4694548.9916.04Pr tors.mode(31)+β(N-C-N)(23) +β(N5-C10-C9)(10)-421418405 2.01 1.44Pr tors.mode(29)+Ring Tors.mode(17)--4103967.608.21Ring Tors.mode(54)(continued)Exp a Exp a Calc.Calc.Calc.Calc.Assignment of dominant IR Raman(Unscaled(Scaled IR Raman modes in order ofWave no.Wave no.Wave no.Wave no.Intensity Intensity decreasing potential in cm−1in cm−1in cm−1)in cm−1)energy distribution(PED)-38138937719.530.39β(O2-C7-N6)(22)+Ring Tors.(21) Tors.(O4-C11-C13-C12)(12)-352364352 3.228.17Tors.(F1-C8-C10-C9)(59) +Tors.(O3-N6-C9-C8)(10)-319312302 1.680.76β(C10-C9-F1)(26)+β(C8-N6-C7)(18) +β(C10-N5-C11)(29)+β(C10-N5-C7)(12)--2872787.10 4.57Ring Tors.(24)+βout(C10-C9-F1)(22) +β(C15-C11-N5)(20)--2432360.17 1.90Pr tors.mode(32)+Ring Tors.(30) +βout(C10-C9-F1)(12)--230223 1.08 1.61Pr tors.mode(30) +β(C10-N5-C11)(29)--166160 4.74 3.08Ring Tors.(64)--152147 2.75 4.58Pr tors.mode(20)+Tors.(C15-C11-N5-C7)(19)+Ring Tors(10)+β(C10-N5-C11)(10)--1281230.78 3.22Tors.(C15-C11-N5-C7)(35)+Ring Tors.(33)+Pr tors.mode(17)--7471 1.78 1.29Tors.(C14-C15-C11-N5)(61) +β(C11-N5-C10)(10)--6159 1.36 1.94Ring Tors.(36)+Tors.(C15-C11-N5-C7)(35)--4543 1.18 1.74Tors.(C11-C7-C10-N5)(67) +Tors.(C12-C11-N5-C7)(11)The experimental IR and Raman data have been taken from http://riodb01.ibase.aist.go.jp/sdbs website.Note:υ:stretching;υs:symmetric stretching;υas:asymmetric stretching;β:in plane bending;βout:out of plane bending;Tors:torsion;sc:scissoring;ωag:wagging;Pr:Five-membered ring;Ring:Hetroaromatic six-membered ring tegafur agree well with the experimental spectral data taken from the Spectral Database for Organic Compounds(SDBS)[16].3.4.1N-H vibrationsThe N-H stretching of hetrocyclic six-membered ring of tegafur is calculated at3477 cm−1.As expected,this is a pure stretching mode and is evident from P.E.D.table con-tributing100%to the total P.E.D.,and is assigned to IR wave number at3426cm−1.The discrepancy in the calculated and experimental N-H stretching wave number is due to the intermolecular hydrogen bonding.The mode calculated at637cm−1represents the pure N-H wagging mode which is assigned well with the peak at646cm−1in Raman spectra.3.4.2C-C and C-H vibrationsC-C stretching are observed as mixed modes in the frequency range1600cm−1to980 cm−1for tegafur with general appearance of C-H and C-C stretching modes and are in good agreement with experimentally observed frequencies.C-C stretches are calcu-lated to be1090,980,934and886cm−1.The functional group region in aromatic het-rocyclic compounds exhibits weak multiple bands in the region3100∼3000cm−1.The six-membered ring stretching vibrations as well as the C-H symmetric and asymmet-ric stretching vibrations of methylene group in tegafur are found in the region3125to 2925cm−1.In the present investigation,the strengthening and contraction of C-H bond C(10)-H(17)=108.147pm in hetrocyclic six-membered ring may have caused the C-H stretching peak to appear at3115cm−1having almost100%contribution to total P.E.D. in calculation.This C-H stretching vibration is assigned to the3076cm−1IR spectra. The calculated peaks at3017,3007,2998cm−1and2967cm−1are identified as methylene asymmetric and symmetric stretching vibrations with more than80%contribution to the total P.E.D.are matched moderately and have been assigned at3033cm−1in the IR and at3004and2976cm−1in Raman spectra respectively.The calculated peaks in the frequency range1475∼1400cm−1of tegafur correspond methylene scissoring modes with more than85%contribution to the total P.E.D.are as-signed at1471/1473and1466/1469cm−1in the IR/Raman spectra.Methylene wagging calculated at1300cm−1(62%P.E.D.),1294and1266cm−1(56%P.E.D.each),show con-siderable mixing with methylene twisting mode,whereas dominant twisting modes are calculated at1257cm−1and1189cm−1with60%and40%contribution to P.E.D.The mode calculated at897,800and705cm−1are identified as methylene rocking with their respective33%,69%and39%contribution to the total P.E.D.3.4.3Ring vibrationsThe calculated modes at868cm−1and722cm−1represent the pure six-membered ring wagging and breathing modes.As expected the skeletal out of plane deformations/ the torsional modes appear dominantly below the600cm−1.The mode calculated at 789cm−1represent mixed mode with(C-C-N)and(C-N-C)in-plane bending and F-C stretching and corresponds to Raman/IR mode at782/773cm−1.The experimental wave number at646cm−1in Raman spectra is assigned to the in-plane(O-C-N)and(F-C-C) bending at647cm−1.3.4.4C=O vibrationsThe appearance of strong bands in Raman and IR spectra around1700to1880cm−1show the presence of carbonyl group and is due to the C=O stretch.The frequency of the stretch due to carbonyl group mainly depends on the bond strength which in turn depends upon inductive,conjugative,field and steric effects.The three strong bands in the IR spectra at 1721,1693and1668cm−1are due to C=O stretching vibrations corresponding to the three C=O groups at C(12),C(8)and C(7)respectively in tegafur.These bands are calculatedat1771,1725and1709cm−1.The discrepancy between the calculated and the observed frequencies may be due to the intermolecular hydrogen bonding.4ConclusionsThe equilibrium geometries of tegafur and5-FU and harmonic frequencies of tegafur molecule under investigation have been analyzed at DFT/6-311+G(d,p)level.In general, a good agreement between experimental and calculated normal modes of vibrations has been was observed.The skeleton of optimized tegafur molecule is non-planar.The lower frontier orbital energy gap and the higher dipole moment values make tegafur the more reactive and more polar as compared to the drug5-FU and results in improved target cell selectivity.The molecular electrostatic potential surface andfirst static hyperpolarizabil-ity have also been employed successfully to explain the higher activity of tegafur over its drug5-FU.The present study of tegafur and the corresponding drug in general may lead to the knowledge of chemical properties which are likely to improve absorption of the drug and the major metabolic pathways in the body and allow the modification of the structure of new chemical entities(drug)for the improved bioavailability. Acknowledgments.We would like to thank Prof.Jenny Field for providing the crystal data of Tegafur and5-FU from Cambridge Crystallographic data centre(CCDC),U.K. and Prof.M.H.Jamroz for providing his VEDA4software.References[1]L.W.Li,D.D.Wang,D.Z.Sun,M.Liu,Y.Y.Di,and H.C.Yan,Chinese Chem.Lett.18(2007)891.[2] D.Engel, A.Nudelman,N.Tarasenko,I.Levovich,I.Makarovsky,S.Sochotnikov,I.Tarasenko,and A.Rephaeli,J.Med.Chem.51(2008)314.[3]Z.Zeng,X.L.Wang,Y.D.Zhang,X.Y.Liu,W H Zhou,and N.F.Li,Pharmaceutical Devel-opment and Technology14(2009)350.[4]ura,A Azucena,C Carmen,and G Joaquin,Therapeutic Drug Monitoring25(2003)221.[5] A.D.Becke,J.Chem.Phys.98(1993)5648.[6] C.Lee,W.Yang,and R.G.Parr,Phys.Rev.B37(1988)785.[7] B.Miehlich,A.Savin,H.Stoll,and H.Preuss,Chem.Phys.Lett.157(1989)200.[8]W.Kohn and L.J.Sham,Phys.Rev.140(1965)A1133.[9]M.J.Frisch,G.W.Trucks,H.B.Schlegel,et al.,Gaussian03,Rev.C.01(Gaussian,Inc.,Wallingford CT,2004).[10] A.P.Scott and L.Random,J.Phys.Chem.100(1996)16502.[11]P.Pulay,G.Fogarasi,G.Pongor,J.E.Boggs,and A.Vargha,J.Am.Chem.Soc.105(1983)7037.[12]R.Dennington,T.Keith,lam,K.Eppinnett,W.L.Hovell,and R.Gilliland,GaussView,Version3.07(Semichem,Inc.,Shawnee Mission,KS,2003).[13]M.H.Jamroz,Vibrational Energy Distribution Analysis:VEDA4Program(Warsaw,Poland,2004).[14]G.Keresztury,S.Holly,J.Varga,G.Besenyei,A.Y.Wang,and J.R.Durig,Spectrochim.Acta49A(1993)2007.[15]G.Keresztury,Raman spectroscopy theory,in:Handbook of Vibrational Spectroscopy,Vol.1,eds.J.M.Chalmers and P.R.Griffith(John Wiley&Sons,New York,2002)pp.1.[16]http://riodb01.ibase.aist.go.jp/sdbs/(National Institute of Advanced Industrial Scienceand Technologys,Japan)[17] D.A.Kleinman,Phys,Rev.126(1962)1977.[18]J.Pipek and P.Z.Mezey,J.Chem.Phys.90(1989)4916.[19]dd,Introduction to Physical Chemistry,third ed.(Cambridge University Press,Cam-bridge,1998).[20] F.H.Allen,O.Kennard,and D.G.Watson,J.Chem.Soc.,Perkin Trans.2(S1)(1987)12.[21] B.Blicharska and T.Kupka,J.Mol.Struct.613(2002)153.[22]I.Fleming,Frontier Orbitals and Organic Chemical Reactions(John Wiley and Sons,NewYork,1976)pp.5-27.[23]J.S.Murray and K.Sen,Molecular Electrostatic Potentials,Concepts and Applications(El-sevier,Amsterdam,1996).[24]I.Alkorta and J.J.Perez,Int.J.Quant.Chem.57(1996)123.[25] E.Scrocco and J.Tomasi,Advances in Quantum Chemistry,Vol.11(Academic Press,NewYork,1978)pp.115.[26] F.J.Luque,M.Orozco,P.K.Bhadane,and S.R.Gadre,J.Phys.Chem.97(1993)9380.[27]J.Sponer and P.Hobza,Int.J.Quant.Chem.57(1996)959.。
风云三号_E_星空间环境载荷综合探测技术
北京大学学报(自然科学版) 第60卷 第1期 2024年1月Acta Scientiarum Naturalium Universitatis Pekinensis, Vol. 60, No. 1 (Jan. 2024)doi: 10.13209/j.0479-8023.2023.096风云三号E星空间环境载荷综合探测技术沈国红1,2,†黄聪3,4张鹏飞5张效信3,4王金华5李佳薇3,4宗位国3,4张珅毅1,2张贤国1,2孙越强1,2杨勇5张焕新1,2邹鸿6王劲东1,2孙莹1,2白超平1,2田峥1,21.中国科学院国家空间科学中心, 北京 100190;2.北京市空间环境探测重点实验室, 北京 100190;3.中国气象局国家卫星气象中心北京市空间天气重点实验室, 北京 100081; 4.许健民气象卫星创新中心, 北京 100081; 5.上海卫星工程研究所, 上海 201109; 6.北京大学地球与空间科学学院, 北京摘要针对中国风云三号卫星运行的低地球太阳同步轨道, 开展空间环境及粒子辐射效应监测, 提出基于空间环境监测器Ⅱ型载荷的综合探测技术。
在各载荷技术指标的地面研制过程中, 通过标准放射源、等效信号源、粒子加速器和标准磁场等不同方式进行标定和实验验证。
结果表明, 多方向全能谱粒子探测的能量范围为30keV~300MeV, 精度优于10%; 磁场强度测量范围为−65023~+65023nT, 精度优于0.73nT; 电位探测范围为−32.4~+23.7kV, 灵敏度优于10V; 辐射剂量探测范围为0~3×104rad(Si), 灵敏度优于8.3rad(Si)。
通过空间环境监测器Ⅱ型载荷对卫星运行轨道上的粒子辐射环境、原位磁场矢量变化、辐射剂量累积以及卫星表面电位变化等进行观测, 可以为航天活动、卫星设计、空间科学研究及空间天气预警预报业务提供必要的数据支撑。
关键词空间环境; 粒子探测; 电位探测; 辐射剂量; 磁场探测Comprehensive Detection Payload Technology for SpaceEnvironment of FY-3E SatelliteSHEN Guohong1,2,†, HUANG Cong3,4, ZHANG Pengfei5, ZHANG Xiaoxin3,4, WANG Jinhua5,LI Jiawei3,4, ZONG Weiguo3,4, ZHANG Shenyi1,2, ZHANG Xianguo1,2, SUN Yueqiang1,2, YANG Yong5, ZHANG Huanxin1,2, ZOU Hong6, WANG Jindong1,2, SUN Ying1,2,BAI Chaoping1,2, TIAN Zheng1,21. National Space Science Center, Chinese Academy of Science, Beijing 100190;2. Beijing Key Laboratory of Space EnvironmentExploration, Beijing 100190; 3. Key Laboratory of Space Weather, National Satellite Meteorological Center, China Meteorological Administration, Beijing 100081; 4. Innovation Center for FengYun Meteorological Satellite (FYSIC), Beijing 100081;5. Shanghai Institute of Satellites Engineering, Shanghai 201109;6. School of Earth and Space Sciences,Abstract To monitor the space environment and its effects in the low-Earth sun-synchronous orbit of China’s FY-Ⅱ3 satellite, a comprehensive detection technology based on the type loads of the space environment monitor isproposed. In the process of ground development, various technical indicators of the space environment compre-hensive detection payload have been calibrated and experimentally verified by different methods such as standard radiation source, equivalent signal source, particle accelerator and standard magnetic field. The results show that the multi-direction full-spectrum particle detection achieves an energy range of 30 keV–300 MeV, with the accuracy of ≤10%. The magnetic field detection realizes the measurement range of −65023–+65023 nT, with the accuracy of ≤0.73 nT. The potential detection realizes the measurement range of −32.4–+23.7 kV, with the sensitivity of ≤10V.The detection of radiation dose realizes the measurement range of 0–3×104 rad (Si), with the sensitivity of ≤8.3 rad国家自然科学基金(41931073)和国家重点研发计划(2021YFA0718600)资助收稿日期: 2023–01–29; 修回日期: 2023–02–28145北京大学学报(自然科学版) 第60卷 第1期 2024年1月146(Si). Through comprehensive observation of particle radiation environment, change of in-situ magnetic field vector, radiation dose accumulation and change of satellite surface potential in satellite operation orbit, the space environ-ment monitor provides necessary data support for space activities, satellite design, space science research and space weather early warning and prediction.Key words space environment; particle detection; potential detection; radiation dose; magnetic field detection风云三号(FY-3)气象卫星是实现全球、全天候、多光谱、三维、定量遥感的我国第二代极轨气象卫星系列, 包括 01 批、02 批、03 批和已规划的04 吉林农业大学批共 4 个批次。
MS2721A手持电池电源式频谱分析仪产品说明书
≤–153 dBm Displayed Average Noise Level T ypical @ 1GHzUnprecedented in handheld battery powered spectrum analyzers, the sensitivity of the MS2721A delivers the ability to measure very low level signals. Coupled with a wide range of resolution bandwidth choices, you can configure the Spectrum Master to meet your most challenging measurement needs.As the spectrum becomes more and more congested,the ability to measure low level signals becomes more and more important not only for interference detectionbut also for wireless system planning.Soft Key Active Function BlockHeadset 2.5 mmSpeakerLAN ConnectorSoft KeysBattery Charger InputOn/Off ButtonDirectional ButtonsDual FunctionKeypadRotary KnobUSB Jack31981Measurement Area Wide RBW & VBW RangeAM/FM DemodChannel PowerACPROBWField StrengthC/ICellular Measurements yes yes yes yes yes WiFi Measurements yesyesyesyesSpectrum Monitoring yes yes Interference DetectionyesyesyesEthernet connection.Commonly needed measurements are built in. These include field strength,occupied bandwidth, channel power, adjacent channel power ratio,AM/FM/SSB demodulation and carrier to interference (C/I) ratio measurements.The MS2721A Spectrum Master has a very wide dynamic range, allowing measurement of very small signals in the presence of much larger signals.These pictures show a measurement of a –114 dBm signal with and without the presence of a –22 dBm signal only 20 kHz away.Measuring a Small SignalWide Dynamic Range — Measuring a small signal in the presence of a very large signal4a signal source removes any question as to the source of the sidebands.Powerline related sidebands on a synthesized signal generatorTypical Phase Noise PerformanceContinuous frequency coverage from 100 kHz to 7.1 GHz gives the wireless professional the performance needed for the most demanding measurements.Whether your need is for spectrum monitoring, WiFi and WiFi5 installation and testing, RF and microwave signal measurements or cellular signalmeasurements, the MS2721A Spectrum Master gives you the tools you need to make the job easier and more productive. The built-in AM/FM/SSB demodulator simplifies the job of identifying interfering signals.5Remote T oolsImagine sitting at your desk while controlling an MS2721A that is miles away,seeing the screen display and operating with an interface that looks exactly like the instrument itself. That is what Remote Tools lets you do.Local Language SupportThe MS2721A features eight languages English, Spanish, German, French,Japanese, Chinese, Italian and Korean, two custom user-defined languages can be uploaded into the instrument using Master Software Tools, supplied with the instrument.Fast Sweep SpeedThe MS2721A can do a full span sweep in ≤900 milliseconds, and sweep speed in zero span can be set from 50 microseconds up to 4294 seconds. This is faster and more flexible than any portable spectrum analyzer on the market today, simplifying the capture of intermittent interference signals.+43 dBm Maximum Safe Input LevelBecause the MS2721A can survive an input signal of +43 dBm (20 watts)without damage, you can rest assured that the MS2721A can survive in even the toughest RF environments.Spectrum MonitoringA critical function of any spectrum analyzer is the ability to accurately view aportion of the RF and microwave spectrum. The MS2721A performs this function admirably thanks to the wide frequency range and excellent dynamic range. A built-in 64 MB compact flash memory module allows thousands of traces to be stored. The external compact flash connector allows additional compact flash memory to expand the trace storage without limit.Limit LinesThe MS2721A includes two types of limit lines, lower limit lines and upper limit lines. Limit lines may be used either for visual reference or for pass/fail criteria by implementing limit alarms. Limit alarm failures are reported if a signal is above the upper limit line or below the lower limit line. Each limit line may consist of up to 40 segments.AM, FM and SSB DemodulationMultiple Language Support6Segmented Limit Linesa standard feature of the MS2721A.Frequency Counter MarkersThe MS2721A Spectrum Master has frequency counter markers withresolution to 1Hz. Tie this capability to an external precision time base to get complementary accuracy.Functions Multiple Marker Display up to six markers on screen, each marker includes a delta marker. Marker TableDisplay a table of up to six marker frequency and amplitude values plus delta marker frequency offset and amplitude.Upper/Lower Limit Fixed and SegmentedEach upper and lower limit can be made up of between one and 40 segments.Smart Measurements Occupied Bandwidth Measures 99.99% to 1% power bandwidth of a spectrum.Channel Power Measures the total power in a specified bandwidth.C/I Measures the carrier to interference ratio in a specified bandwidth.ACPR Measures power levels in the channels immediately above and below the center channel.Field StrengthUses antenna calibration tables to measure dBm/meter or dBmV/meter.AM/FM/SSB DemodulationAllows the user to listen to interfering signals. De-emphasis is included for narrow-band FM and wideband FM. Upper Sideband and Lower Sideband demodulation includes a BFO that can be tuned ±10 kHz from the center frequency.Multiple Markers plus Multiple Delta Markers7simplifying the capture of intermittent interference signals.Carrier to Interference MeasurementAs more 802.11 access points are installed, there is an increasing level ofinterference in the 2.4 GHz and 5.8 GHz bands occupied by this service and other devices such as cordless telephones. This measurement capability makes it simple for an access point installer to determine if the level of interference is sufficient to cause difficulty for users in the intended service area, and can show the need to change to another access channel. The wide frequency coverage of the MS2721A makes this the only spectrum analyzer you need to install and maintain 802.11a, 802.11b and 802.11g wireless networks.Occupied BandwidthThis measurement determines the amount of spectrum used by a modulated signal.You can choose between two different methods of determining bandwidth: the percent of power method or the “x” dB down method, where “x” can be from 3dB to 100 dB down the skirts of the signal.Adjacent Channel Power RatioA common transmitter measurement is that of adjacent channel leakagepower. This is the ratio of the amount of leakage power in an adjacent channel to the total transmitted power in the main channel, and is used to replace the traditional two-tone intermodulation distortion (IMD) test for system non-linear behavior.The result of an ACPR measurement can be expressed either as a power ratio or a power density. In order to calculate the upper and lower adjacent channel values, the MS2721A allows the adjustment of four parameters to meet specific measurement needs: main channel center frequency, measurement channel bandwidth, adjacent channel bandwidth and channel spacing. When an airinterface standard is specified in the MS2721A, all these values are automatically set to the normal values for that standard.Occupied Bandwidth8Tuning Resolution 1 HzFrequency Reference Aging±1 ppm/yearAccuracy±1 ppm (25°C ±25°C) + long term driftFrequency Span10 Hz to 7.1 GHz plus 0 Hz (zero span)Span Accuracy Accuracy±1 ppm (25°C ±25°C) + long term driftSweep Time minimum 100ms, 50µs in zero spanSweep Time Accuracy±2% in zero spanSweep Trigger Free run, Single, Video, ExternalResolution Bandwidth(–3 dB width) 10 Hz to 3 MHz in 1-3 sequence ±10%, 8 MHz demodulation bandwidthVideo Bandwidth(–3 dB) 1 Hz to 3 MHz in 1-3 sequenceSSB Phase Noise–100 dBc/Hz max at 10, 20 and 30 kHz offset from carrier–102 dBc/Hz max at 100 kHz offset from carrierInput Damage Level≥10 dB attenuation, >+43 dBm, ±50 Vdc<10 dB attenuation , >+23 dBm, ±50 VdcInput protection relay opens at >30 dBm with ≥10 dB input attenuationand at approximately 10 to 23 dBm with <10 dB attenuationRF Input VSWR 2.0:1 maximum, 1.5:1 typical (≥10 dB attenuation)Reference Level Adjustable over amplitude rangeESD Damage Level>10 kV ≥10 dB attenuationAbsolute amplitude accuracyPower levels ≥–50 dBm, ≥35 dBinput attenuation, preamp off100 kHz to ≤10 MHz ±1.5 dB>10 MHz to 4 GHz ±1.25 dB>4 GHz to 7.1 GHz ±1.75 dBSecond Harmonic Distortion(0 dB input attenuation, –30 dBm input)–50 dBc, 0.05 to 0.75 GHz–40 dBc, >0.75 to 1.05 GHz–50 dBc, >1.05 to 1.4 GHz–70 dBc, >1.4 to 2 GHz–80 dBc, >2 GHz9Displayed Average Noise LevelDANL in 10 Hz RBW, 0 dB attentuationreference level –50 dBmFrequency Preamp OnTypical Max10 MHz to 1 GHz–153dBm–151dBm>1 GHz to 2.2 GHz–150dBm–149dBm>2.2 GHz to 2.8 GHz–146dBm–143dBm>2.8 GHz to 4.0 GHz–150dBm–149dBm>4.0 GHz to 7.1 GHz–148dBm–146dBm Noise Figure (Derived from DANL measurement)0 dB attenuation, reference level–50 dBm, 23°C, preamp onFrequency Typical10 MHz to 1.0 GHz11 dB>1 GHz to 2.2 GHz14 dB>2.2 GHz to 2.8 GHz18 dB>2.8 GHz to 4.0 GHz14 dB>4.0 GHz to 7.1 GHz16 dBDisplay Range 2 to 15 dB/div in 1 dB steps. Ten divisions displayed.Amplitude Units Log Scale modes: dBm, dBV, dBmv, dBµVLinear Scale modes: nV, µV, mV, V, kV, nW, µW, mW, W, kW Attenuator Range0 to 65 dBAttenuator Resolution 5 dB stepsInput-Related Spurious–60dBc max*, (<–70 dBc typical), –30 dBm input, 0 dB RF attenuation *Exceptions:Input Frequency Spur Level1674MHz–46 dBc max (–56 dBc typical), 0 to 2800 MHz>1674 to 1774 MHz–50 dBc max (–60 dBc typical) at (F input– 1674 MHz)Residual Spurious, Preamp Off(RF input terminated, 0dB RF attenuation)–90 dBm max**, 100 kHz to <3200 MHz–84 dBm max**, 3200 to 7100 MHz**Exceptions:Frequency Spur Level250, 300 and 350 MHz–85 dBm max~4010 MHz–80 dBm max (–90 dBm typical)~5084 MHz–70 dBm max (–83 dBm typical)~5894 MHz–75 dBm max (–87 dBm typical)~7028 MHz–80 dBm max (–92 dBm typical)Residual Spurious, Preamp On: –100 dBm max(RF input terminated, 0dB RF attenuation)10DisplayBright Color Transmissive LCD, Full SVGA, 8”LanguagesBuilt-in English, Spanish, French, German, Japanese, Chinese, Italian and Korean. Theinstrument also has the capability to have customized languages installed from Master SoftwareTools.Marker ModesSix Markers, Seven Modes: Standard, Delta, Marker to Peak, Marker to Center, Marker toReference Level, Next Peak Left, Next Peak Right, All Markers Off, Noise Marker, FrequencyCounter Marker (1 Hz resolution)SweepsFull span, Zero span, Span Up/Span DownDetectionPeak, RMS, Negative, SampleMemoryTrace and Setup storage is limited only by the capacity of the installed Compact Flash card.For a 256 MB card, storage is greater than 5000 traces and 5000 setups.T racesDisplayed Traces: Three traces with trace overlay. One trace is always the live data, two tracescan be either stored data or traces which have been mathematically manipulated(such as C=A–B).InterfacesType N female RF ConnectorBNC female connectors for external frequency reference and external triggerMini-B USB 2.0 for data transfer to a PCRJ45 connector for Ethernet 10/100-BaseT2.5mm 3-wire headset connectorSize and WeightSize: 12 x 7 x 2.4 in. (313 x 211 x 77mm)Weight: <6.4 lbs. (2.9kg) (typical)EnvironmentalMIL-PRF-28800F Class 2Operating: –10°C to 55°C, humidity 85% or lessStorage: –51°C to 71°CAltitude: 4600 meters, operating and non-operatingSafetyConforms to EN 61010-1 for Class 1 portable equipment.Electromagnetic CompatibilityMeets European Community requirements for CE marking.Specifications are subject to change without notice.11Ordering InformationModel: MS2721A - Handheld Spectrum Analyzer100 kHz to 7.1 GHzStandard Accessories10580-00103User’s Guide61382Soft Carrying Case40-168AC – DC Adapter806-62Automotive Cigarette Lighter/12 Volt DC Adapter 2300-498Master Software Tools CD ROM2000-1360USB A-mini B cable2000-1371Ethernet Cable633-44Rechargeable battery, Li-Ion2000-135864 MB Compact Flash Memory Module64343Tilt Bail1091-172Adapter, N(m) to B(f), 50Ω1091-27Adapter, N(m) to SMA(f), 50ΩOne Year WarrantyCertificate of Calibration and ConformanceOptional Accessories42N50A-3030 dB, 50 Watt, Bi-directional, DC to 18 GHz,N(m)to N(f) Attenuator34NN50A Precision Adapter, DC to 18 GHz, 50Ω,N(m) to N(m)34NFNF50Precision Adapter, DC to 18 GHz, 50Ω, N(f) to N(f) 15NNF50-1.5B Test port cable, armored, 1.5 meter N(m) to N(f)18 GHz15ND50-1.5C Test port cable armored, 1.5 meter, N(m) to7/16 DIN(m), 6.0 GHz15NDF50-1.5C Test port cable armored, 1.5 meter, N(m) to7/16 DIN(f), 6.0 GHz510-90Adapter, 7/16 DIN(f) to N(m), DC to 7.5 GHz, 50Ω510-91Adapter, 7/16 DIN(f)-N(f), DC to 7.5 GHz, 50Ω510-92Adapter, 7/16 DIN(m)-N(m), DC to 7.5 GHz, 50Ω510-93Adapter, 7/16 DIN(m)-N(f), DC to 7.5 GHz, 50Ω510-96Adapter 7/16 DIN(m) to 7/16 DIN(m),DC to 7.5 GHz, 50Ω1030-86Band Pass Filter, 800 MHz band, 806-869 MHz,Loss = 1.7 dB, N(m)-SMA(f)1030-87Band Pass Filter, 900 MHz band, 902-960 MHz,Loss = 1.7 dB, N(m)-SMA(f)1030-88Band Pass Filter, 1900 MHz band, 1.85-1.99 GHz,Loss = 1.8 dB, N(m)-SMA(f)1030-89Band Pass Filter, 2400 MHz band, 2.4-2.5 GHz,Loss = 1.9 dB, N(m)-SMA(f)510-97Adapter 7/16 DIN(f) to 7/16 DIN(f), 7.5 GHz61382Soft carrying case40-168AC/DC adapter806-62Automotive Cigarette Lighter/12 Volt DC Adapter 760-229Transit Case for Anritsu MS2721A HandheldSpectrum Analyzer2300-498Anritsu Master Software Tools CD ROM10580-00103Anritsu HHSA User’s Guide, Model MS2721A 10580-00104Anritsu HHSA Programming Manual,Model MS2721A10580-00105Anritsu HHSA Maintenance Manual,Model MS2721A633-44Rechargeable battery, Li-Ion2000-1374Dual External, Li-Ion charger with universalpower supply2000-1030Portable antenna, 50Ω, SMA(m) 1.71-1.88 GHz 2000-1031Portable antenna, 50Ω, SMA(m) 1.85-1.99 GHz 2000-1032Portable antenna, 50Ω, SMA(m) 2.4-2.5 GHz2000-1035Portable antenna, 50Ω, SMA(m) 896-941 MHz 2000-1200Portable antenna, 50Ω, SMA(m) 806-869 MHz 2000-1361Portable antenna, 50Ω, SMA(m) 5725-5825 MHz 2000-135864 MB Compact Flash Memory ModuleDirectional Antennas2000-1411Portable Yagi antenna, 10 dBd, N(f) 822-900 MHz 2000-1412Portable Yagi antenna, 10 dBd, N(f) 885-975 MHz 2000-1413Portable Yagi antenna, 10 dBd, N(f) 1.71-1.88 GHz 2000-1414Portable Yagi antenna, 9.3 dBd, N(f) 1.85-1.99 GHz 2000-1415Portable Yagi antenna, 10 dBd, N(f) 2.4-2.5 GHz 2000-1416Portable Yagi antenna, 10 dBd, N(f) 1.92-2.23 GHzDiscover What’s Possible®©Anritsu January 2005. All trademarks are registered trademarks of their respective companies.Data subject to change without notice. For more recent specifications visit 11410-00332, Rev. CSALES CENTERS:United States (800) ANRITSUCanada (800) ANRITSUSouth America 55 (21) 2527-6922Europe 44 (0) 1582-433433Japan 81 (46) 223-1111Asia-Pacific (852) 2301-4980Microwave Measurement Division490 Jarvis Drive, Morgan Hill, CA 95037-2809。
waters质谱masslynx软件使用说明
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Micromass UK Limited believes that the information in this publication is accurate. However the information is subject to change without notice and should not be construed as a contractual undertaking by Micromass UK Limited. Despite the care that has been given to the preparation of this publication, Micromass UK Limited accepts no responsibility for any loss or any other matter that may arise from any error or inaccuracy that may inadvertently have been included. Copyright 1993-2002 Micromass Ltd. All Rights Reserved. No part of this publication may be copied without the express written permission of Micromass UK Limited.
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MassLynx NT Users Guide
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MassLynx NT User’s Guide............................................................................
Comment on `Anomalously Large Gap Anisotropy in the a-b Plane of Bi$_2$Sr$_2$CaCu$_2$O$_{8+
a rXiv:c ond-ma t/94173v131Jan1994Comment on “Anomalously Large Gap Anisotropyin the a-b Plane of Bi 2Sr 2CaCu 2O 8+δ”Kazumasa Miyake and Osamu NarikiyoDepartment of Material Physics,Faculty of Engineering ScienceOsaka University,Toyonaka 560,Japan (February 1,2008)79.60.Bm,73.20.Dx,74.72.HsTypeset using REVT E XIn a recent Letter[1],Shen and collaborators reported that angle-resolved photoemission spectra(ARPES)in Bi-2212cuprate superconductor far below T c has anomalously large anisotropy and then concluded that the symmetry of Cooper pair is likely to be d x2−y2,i.e.,∆k=∆(cos k x a−cos k y a)[2].In this Comment we point out that the interpretation done by Shen et al.,where the shift of edge near Fermi level has been identified with the gap ∆k,is not unambiguous,and that a possibility of d xy pairing,i.e.,∆k=2∆sin k x a sin k y a, cannot be ruled out.The ARPES intensity is proportional to A(k,ω)≡−1/π·Im G R(k,ω)given in the superconducting state as follows:A(k,ω)=z k −ω−˜ξkπ ˜γk(ω−˜E k)2+˜γ2k+A inc(k,ω),(1)where z k is the renormalization amplitude,˜E k≡(∆2k+˜ξ2k)1/2and˜γk being the dispersion and damping of quasiparticles.Thefirst term of Eq.(1)gives coherent contribution due to quasiparticles and the second term,A inc(k,ω),represents incoherent background.In the photoemission experiment(ω<0),thefirst term in the coherent part,if it exists,gives dominant contribution.First of all,it is remarked that the peak position of the coherent component is shifted downward by amount of(∆2k+˜ξ2k)1/2+˜ξk when the superconductivity sets in.The maximum gap2∆at T=0is related to the transition temperature T c as2∆(0)≃3.5k B T c if it is estimated by the weak coupling treatment assuming d x2−y2pairing.Since T c=78K and then the maximum gap2∆(0)≃2.7×102K,such a shift of peak position should be detectable there far below T c within their relative experimental resolution of∼5meV[1].Secondly,the damping rate of quasiparticles in the normal state is given roughly as ˜γ≃[(k B T)2+(ω/π)2]1/2[3].Therefore,narrowing of the coherent peak aroundω∼−30meV, which are the case in a typical example of Fig.1in Ref.[1],seems to be detectable when the temperature is decreased from85K down to20K provided wave number k is located at the position such that∆k=0.Thirdly,the spectral weight just below the Fermi level in the superconducting state is half of that in the normal state if|˜ξk|is much less than∆k.This is because half of the spectral weight of normal quasiparticles is transferred to above the Fermi level due to gap ly,ARPES intensity of coherent part in the superconducting state near the Fermi level is rather harder to observe than in the normal state if the gap∆k takes maximum there.Now we encounter difficulty in interpretation of Ref.[1].The ARPES at the location A on Γ-¯M line in Fig.1does not show visible shift of peak position at all,but exhibits narrowing of the peak width suggesting a separation of coherent peak and incoherent background. If the gap had maximum at A,the peak should have shifted downward about15meV in contrary to the observation in Fig.1.Therefore,as an alternative interpretation,it seems more appropriate to consider that the gap∆k vanishes along the k x-axis(k y=0),parallel to Cu-O bond,and that we observed the narrowing of the coherent peak atω=˜ξk which had been located just below the Fermi level at˜ξk∼−30meV.The present interpretation is also consistent with the so-called aging effect reported in Ref.[1],because the inhomogeneity of the surface caused by deficit of oxygen or so is expected to give an excess of damping of quasiparticles leading to broadening of the coherent peak.On the other hand,at the location B onΓ-Y line,where the coherent component is hardly seen in the normal state(note that the maximum intensity at A and B in the normal state are almost the same while the incoherent background at B is larger than that at A by 30-40%),there appears a peak aroundω∼−30meV far below T c without showing apparent shift of the edge near the Fermi level.If the gap vanished at B as interpretted in Ref.[1],the narrowing of the coherent peak should have been observed.The intensity profile at B in Fig. 1rather looks as if new peak is added to the incoherent background when the temperature is decreased far below T c.So it seems more natural to consider that B is located just at or above the Fermi level and a new peak appeares aroundω=−˜E k≃−30meV but with a reduced weight z k(−˜ξk+˜E k)/2˜E k<z k/2.In conclusion,ARPES data of Ref.[1]are also understood even if we assume d xy pairing which has gap vanishing alongΓ-¯M line and reaching maximum around B.Theoretical arguments favoring such pairing in cuprates have been put forth in various contexts[4,5]. Kane et al.has also suggested in a very recent Letter[6]that results of scanning tunneling microscope in Bi-2212sample are understood on the basis of d xy pairing[7].REFERENCES[1]Z.-X.Shen,D.S.Dessau,B.O.Wells,D.M.King,W.E.Spicer,A.J.Arko,D.Marshall,L.W.Lombardo,A.Kapitulnik,P.Dickinson,S.Doniach,J.DiCarlo,A.G.Loeser,andC.H.Park,Phys.Rev.Lett.70,1555(1993).[2]T.Takahashi has recently succeeded in reproducing qualitatively the same ARPES asRef.[1]by somewhat different method.(private communication)[3]T.Ito,K.Takenaka,and S.Uchida,Phys.Rev.Lett.70,3995(1993),and referencestherein.[4]P.B.Littlewood,C.M.Varma,and E.Abrahams,Phys.Rev.Lett.63,2602(1989).[5]O.Narikiyo and K.Miyake,Solid State Commun.,in press.[6]J.Kane,Q.Chen,and K.-W.Ng,and H.-J.Tao,Phys.Rev.Lett.72,128(1994).Notethat k x-axis in their paper is at an angle of45◦measured from Cu-O ly,the pairing of the type∆(θ)=∆0(cos k x a−cos k y a)in their paper has d xy-symmetry in a frame of reference in the present Comment where k x-axis is parallel to the Cu-O bond.[7]For YBCO,M.Sato et al.has observed an aspect suggesting the d xy pairing similarly toRef.[6](private communication).。
核磁共振分子运动学分析实验指导说明书
Diffusion experiments with Vnmrj 2.2C and 2.2D.E. Alvarado. University of Michigan. 04/12/10The diffusion coefficient of a molecule in solution depends on its effective molecular weight, size and shape, and can be used to estimate its relative molecular size (its hydrodynamic radius). It has applications in organic and inorganic chemistry3,5, for example to determine molecular weight in polymers, biopolymers and other aggregated materials. It can also be used to study molecular interactions and complexation processes in chemistry and to determine association constants. Recently, a method to estimate the molecular mass of small molecules in dilute aqueous and organic solutions was developed8.The present manuscript refers to diffusion experiments with Vnmrj 2.2C and 2.2D and Chempack 4.1. The software contains several pulse sequences for different experiments. Check the Vnmr manual for details. Here we will use the the pulse sequence DgcsteSL_cc (DOSY gradient compensated stimulated echo with spin lock and convection compensation), which is an enhancement of the classical PGSE (Pulsed Gradient Spin-Echo) pulse sequence.The PGSE pulse sequence, as originally proposed by Stejskal and Tanner 40 years ago is perhaps the easiest to understand, see the Figure 1 below. Briefly, after applying a 90° pulse, the nuclear spins of the sample will start precessing along the main magnetic field and dephase according to their absorption frequencies at this field. Then, a magnetic field gradient of strength gzlvl1 and duration gt1 is applied along the z axis of the tube and the spins will now be dephased due to their location in the gradient. After a short delay, a 180° pulse is applied that has the effect of inverting the precession direction. If the spins have not undergone translational motion along the z axis, the second applied gradient will be identical to the first, canceling its effect and the spins refocus (produce a spin- echo). However, if there was motion the effective magnetic field experienced by the spins during the second gradient will be different to the first and the spins will not completely refocus. The resulting signal will have a decreased intensity. The amount of attenuation is proportional to the displacement along the z axis, the gradient strength and the diffusion delay. Many other, more complex pulse sequences are available6,10,11, with portions aimed at increasing sensitivity and reducing artifacts, but they all follow the same principle.Figure 1. Classic PGSE pulse sequence.To measure molecular diffusion in a solution, a series of spectra with increasing gradient strengths must be recorded, Figure 2. By fitting the intensity (or integration) of the peaks to the Stejskal-Tanner function as described later, the diffusion constants can be calculated. And from the diffusion coefficients it is possible to calculate the hydrodynamic radius via the Stokes-Einstein equation2.This document contains only enough information to setup a basic experiment with Varian's Vnmrj software and analyze the results. Extensive discussions of diffusion experiments and its applications can be found in thechemical literature, in the references below and in advanced NMR texts.Figure 2. Sections of a DgcsteSL_cc experiment of a solution of sucrose in D2O. The anomeric hydrogen of sucrose at 5.42 ppm is shown on the left while the residual HDO signal at 4.79 ppm is shown on the right. Notice the sigmoidal shape of the decay and how the HDO signal decays faster.Experiment setupSome recommendations: If your solvent is organic, it is advisable to have TMS in solution so it can be used as a reference in the calculation8. If it is D2O, the residual solvent signal (HDO) can be used as the reference. It is very important to regulate and have a very stable and homogeneous temperature. Extreme (low and high) temperatures may produce convection currents inside the tube that are difficult to avoid and lead to errors. During the experiment, the parameters should be chosen so that the intensities of the signals of interest decay from 100% to about 20%.After inserting the sample and loading the shims, shim the magnet quickly (you will need to reshim later) and take a quick spectrum. Reduce the spectral width to your sample's needs and take a new spectrum. Display the optimized spectral width, transmitter offset, and gain (type sw?tof?gain?) and write down the results. When measuring diffusion on nuclei other than proton, the following parameters are also reset by the setup macro and the correct values will need to be reentered: tn, dn, tpwr and pw (set pw to the 90º value of the nucleus you want to measure). From the Experiments menu or from the Experiment Panel (on the Holding tab at the left side of vnmrj) select DgcsteSL_cc. Set sw, tof and gain to the values you just found (and do the same for the other parameters if the nucleus is not H1). Set the desired temperature, for example by typing “temp=25 su” on the command line, and while the temperature is stabilizing, adjust the remaining parameters that follow. Most of the parameters can be set from the Acquire, Pulse Sequence panel shown below.Of particular importance for this experiment are three parameters. The D iffusion delay (del) is the amount of time allowed for the molecules to diffuse. Larger molecules will move slower and may require long periods of time for an accurate measurement, while small molecules move faster and require short diffusion delays. If the diffusion delay is set too short, the peaks will not have enough time to decay sufficiently for an accurate determination; and if it is too long, the signals will decrease in intensity to zero well before the end of the experiment and the last few spectra will contain only noise. Additionally, the diffusion delay should not be too long because signal intensity also decreases due to relaxation during this delay and thermal convection processes have more time to interfere with the experiment. It is for those reasons that in general the diffusion delay should be between 50 and 200 ms. If more time is required, it is better to increase the diffusion gradient length (gt1) instead. For example, a gradient length of 2 ms with a delay of 400 ms is equivalent to a gradient of 4 ms with a delay of 200 ms. Good values to start for medium size organic molecules in low viscosity solvents are: diffusion gradient length = 2 ms, diffusion delay = 200 ms. Double the gradient length for water and other viscoussolvents. Change the values of these parameters in the parameter panel as shown.For this and other diffusion experiments we have to collect a series of spectra where the diffusion gradient (whose length we just defined above) has increasing gradient strengths. This is accomplished by setting up in an array the values of the Diffusion gradient level (gzlvl1) from 0 to the maximum value allowed by the gradient amplifier. In our Inovas and 400MRs the maximum value is 2048. These numbers are in an arbitrary scale without units provided by a digital-to-analog converter (DAC). The calibration for these DAC numbers to gauss/cm was performed by the NMR Facility staff and is shown in the parameter panel as “DAC to G”. For example, in our Inova 500 with the “id” probe, DAC_to_G has been calibrated with D2O at 25 °C and has a value of 0.00961 gauss/cm·DAC. Thus the maximum gradient for this probe/instrument is 19.7 gauss/cm or 1.97 T/m. To setup the array you can either click on [Setup coarse gradient array] or on [Setup DOSY using conditions above]. The first sets up an array of only 8 gradients while the second sets up an array using the Number of increments shown above (15 is the default). The coarse array is useful for running a quick experiment to determine if the diffusion delay and diffusion length are appropriate to the sample.Before starting the experiment select Alternate gradient signs on odd scans and Lock gating during gradients. If solvent presaturation is needed, check one of the options d1 only, del only or both and set the saturation frequency (it has to be determined before this experiment in a presaturation experiment). Do not increase the power to more than 5. Set the number of scans desired (nt), the relaxation delay (d1) and check the experimental time. When everything is what you want, click on [Acquire] to start the acquisition. ProcessingMost of the processing can be done from the Process, DOSY process panel shown below. First, enable a line broadening of 0.3 or 0.5 and click on [Process all spectra]. Carefully phase the first spectrum and verify that the phasing is consistent for all spectra in the array using the buttons. Select integral mode and manually cut the integral into regions. Apply a baseline correction to all the spectra in the array with [Baseline correct all spectra]. This step is very important to obtain more accurate peak intensities or integrals. Select the peaks to use in the calculation with the minimum threshold tool . When you click on [Calculate full DOSY] the calculations will be performed and the results displayed in tabular form and a 2D dosy spectrum will be shown. Notice that the calculation is always done with the value of DAC_to_G that was read from the configuration files when the spectrum was acquired. If you run your own calibration and want to re-calculate the diffusioncoefficients using your own value, click on [Recall original NMR spectra] and then, on the command line type: setvalue('DAC_to_G', your_gcal, 'processed') where your_gcal is your DAC_to_G calibration. Then click on [Calculate Full DOSY] again.Also notice that if the 2D display is being shown and you click on [Calculate Full DOSY] again, the data gets corrupted and you will have to reload and reprocess you spectrum again. If you want to recalculate a different section of the spectrum or use different parameters, click on [Recall original NMR spectra] first.After the calculation, you can display the line fitting of an individual peak in the spectrum to the Stejskal-Tanner equation by entering a peak number in Peak #_ and clicking on [Show fit for Peak # above]. The actual data will be shown along with the fitted curve and a curve showing the differentials between the two. This is useful to determine if one or more of the individual spectra contains data that deviates considerably from the trend and may need to be discarded. When this happens, the [Calculate Full DOSY with dialog] can be useful. This button allows individual spectra to be omitted from the analysis. Remember to click on [Recall original NMR spectra] first.According to the manual, the Calibration Flag option corrects systematic errors in the experiment. Unfortunately, the manual doesn't mention how these errors are corrected.In general, the interface to this one and other diffusion experiments is very buggy; be cautious. For example, the “Fiddle” buttons (for deconvolution) do not work. The Use Integral Values option does not work. And do not click on the [Plot DOSY] button; not only it doesn't work, but it also freezes Vnmrj.Manual analysisWhile Vnmrj's analysis routines give you a quick and easy way to calculate diffusion coefficients from the spectra, you will get better control of the analysis by measuring peak heights or integrals and doing your own calculations. Stejskal and Tanner have shown that the intensity of the signals in diffusion experiments is described by the following equation:ln(I/I0) = -γ2 δ2 G2(∆ - δ/3) Dwhere:I = intensity or integral of the peak at a given GI0 = intensity or integral of the peak at G = 0γ = magnetogyric constant of the nucleus (for 1H, γ = 2.675 x 108 T-1 s-1 )δ = diffusion gradient length (parameter gt1)∆ = diffusion delay (parameter del)G = gradient field strength (gzlvl1[n] * DAC_to_G)D = diffusion coefficientWith the list of integrals or intensities, a Stejskal-Tanner attenuation plot can be constructed (see Figure 3). This is a plot of ln(I/I0) vs. G2 , and from the slope of this plot the diffusion coefficient D can be extracted. Alternatively, the data can also be fitted directly to the equation I = I0 exp[ -(γδ g)2 (∆ – δ/3) D] using line fitting programs like QtiPlot, Origin, Scientist, SigmaPlot, etc.Figure 3. Stejskal-Tanner plot of a solution of a ruthenium coordination complex in CD2Cl2 at25 C. From the plot, the diffusion coefficients of TMS and of the compound were measured as23.3x10-10 and 9.0x10-10 m2/s respectively. Having TMS in the solution allows the determination ofthe solution's viscosity and of the compound's hydrodynamic radius8. The measured compound'sradius gives an insight into its dimerization process (A ↔ AA).To produce a list of integrals, transform the spectra, select integral regions, carefully correct the bias and slope of the integrals and perform baseline correction as described before. Display the Process, Integration panel (shown below), select Partial under Integral Display Mode, position vnmrj's cursor on top of one of the integrals, select Single Peak under Normalize Area To:, type in a number in Integral Area and click on [Set Integral Value]. The list of integrals for the current spectrum only, normalized to the value entered will be shown on the right side of the panel. You can now generate a list of integrals for all the spectra with the macro UMdli. With this macro you can have the list printed or emailed to you in a format convenient to copy and paste to a line fitting program.With the difussion coefficient, the hydrodynamic radius of a compound in solution can be calculated from the Stokes-Einstein equation:r H =kbT 6 Dwherek b = Boltzman constant, 1.3806 x 10-23 kg m2 s-2 K-1T = temperatureη = viscosity of the solution at temperature TD = diffusion coefficientCalibrationThe parameter DAC_to_G must be calibrated to do the calculations. This parameter is a conversion for the units of the gradient amplifier (DAC units) to gradient in gauss/cm. The parameter has already been calibrated in our spectrometers but you may wish to verify it or recalibrate it yourself. This is done with a sample of known diffusion coefficient like HDO in D2O (the residual solvent peak in D2O). Regulate the temperature and allow at least 10 minutes to equilibrate, run a diffusion experiment and after Fourier transformation and baseline correction select Use Peak Heights, expand the region around the HDO peak and type“dosy_grad_calib” to recalibrate. The macro will ask for the expected value of the peak in units of 10-10m2/s (e.g., for HDO at 25 °C enter 19.02). Known values4 can be found in the table below. Use a diffusion gradient length of 2 ms, a diffusion delay of 100 ms and a long relaxation delay of at least 10 seconds for D2O at 25 °C (it is better to use D2O doped with 0.1 mg/mL GdCl3 so that a shorter delay can be used). TypeDAC_to_G? to print the new calculated value.Sample Diffusion coefficient410% D2O in 90% H2O at 25 °C22.7 x10-10 m2/sHDO in D2O at 5 °C10.34 x10-10 m2/sHDO in D2O at 25 °C19.02 x10-10 m2/sHDO in D2O at 45 °C30.27 x10-10 m2/ssucrose in D2O at 25 °C 4.4 x10-10 m2/s (this lab 01/18/10)References[1] C.S. Johnson Jr. Prog. Nucl. Mag. Res. Spectrosc.34, 203-256 (1999).[2]P.S. Pregosin. Prog. Nucl. Mag. Res. Spectrosc.49, 261-288 (2006)[3]Y. Cohen, L. Avram and L. Frish. Angew. Chem. Int. Ed.44, 520-554 (2005)[4] B. Antalek. Concepts Magn. Reson. 14, 225-258 (2002)[5][P.S. Pregosin, P.G. Anil Kumar and I. Fernandez. Chem. Rev.105, 2977-2998 (2005)[6]M.D. Pelta, H. Barjat, G.A. Morris, A.L. Davis and S.J. Hammond. Magn. Reson. Chem. 36, 706-714(1998).[7]Chemical Properties Handbook. C.L. Yaws, Ed. McGraw-Hill 1999. (online access;/knovel2/Toc.jsp?BookID=49)[8] C. A. Crutchfield and D. J. Harris. J. Magn. Reson.185, 179-182 (2007)[9]Stefano Chimichi in http://www.chimorg.unifi.it/public/chimichi/nmrsolv.html[10]Varian manual, Vnmrj 2.2C: “NMR Spectroscopy, User Guide” Chapter 10.[11]J.C. Cobas, P. Groves, M. Martín-Pastor, A. De Capua. Curr. Anal. Chem. 1, 289-305 (2005). Appendix 1. Useful constantsSolvent Temp,°C Viscosity (η), kg · s-1 · m-1D2O20 1.2467 x 10-325 1.095 x 10-3H2O20 1.0016 x 10-3250.8909 x 10-3CDCl325?0.55 x 10-3200.57 x 10-3CD2Cl2250.417 x 10-3200.436 x 10-3CH3OH200.59 x 10-3CD3OD200.52 x 10-3 Acetone-d6200.34 x 10-3 DMSO-d620 2.4 x 10-3 Toluene-d8200.58 x 10-3 Benzene-d6200.69 x 10-3 Acetonitrile-d3200.39 x 10-3 Pyridine-d5200.97 x 10-3From http://www.chimorg.unifi.it/public/chimichi/nmrsolv.html and other sources.Some conversion constants:1 Pa·s (Pascal-second) = 1 kg s-1 m-11 P (1 poise) = 1 g·cm−1·s−1.The relation between poise and pascal-seconds is:10 P = 1 kg·m−1·s−1 = 1 Pa·s,1 cP = 0.001 Pa·s = 1 mPa·s.Appendix 2. For versions previous to vnmrj 2.2C/chempack 4.1.Earlier versions of vnmrj contain even more bugs than 2.2C; be careful. Essentially you can follow the same procedures described here but you will have to enter all parameters manually. The full list of parameters and other information about the experiment can be found in the manual page (go to the Process/Text Output panel and click on [Sequence Manual] ). Run DgcsteSL_cc and verify or modify the parameters (suggested starting values are in parenthesis):Parameter Typical value Commentdel0.1-0.5 (0.2)diffusion delay (in seconds)gt10.001-0.005 (0.002)Diffusion gradient length (in seconds)gzlvl110-2000Diffusion gradient level, arrayed (in dac units)d13-5 (5.0)relaxation delay (seconds)nt8*n (8)number of transientsspin0sample spinning must be offss8steady state transientslb0.5line broadeningSet up a linear array of gzlvl1 values (Menu: Acquisition>Parameter arrays). Typically 20 values, from 10 to 2000 in increments of 100. In principle, the first value should be 0 but in practice this value gives unpredictable results; use 10 instead. Use the command array('gzlvl1', 20, 0, 100)gzlvl1[1]=10 to setup the array or set it up from the menu Acquisition > Parameter Arrays.When the experiment is finished, transform and phase the first or second spectrum. Integrate the spectrum and define all integration regions (even those not needed). Apply a baseline correction to all the spectra in the array manually or with UMbc. Normalize one region to 1 or to 100 and create a list of integrals for all the spectra in the array with the UMdli macro. Process the data manually.。
3GPP TS 36.331 V13.2.0 (2016-06)
3GPP TS 36.331 V13.2.0 (2016-06)Technical Specification3rd Generation Partnership Project;Technical Specification Group Radio Access Network;Evolved Universal Terrestrial Radio Access (E-UTRA);Radio Resource Control (RRC);Protocol specification(Release 13)The present document has been developed within the 3rd Generation Partnership Project (3GPP TM) and may be further elaborated for the purposes of 3GPP. The present document has not been subject to any approval process by the 3GPP Organizational Partners and shall not be implemented.This Specification is provided for future development work within 3GPP only. The Organizational Partners accept no liability for any use of this Specification. Specifications and reports for implementation of the 3GPP TM system should be obtained via the 3GPP Organizational Partners' Publications Offices.KeywordsUMTS, radio3GPPPostal address3GPP support office address650 Route des Lucioles - Sophia AntipolisValbonne - FRANCETel.: +33 4 92 94 42 00 Fax: +33 4 93 65 47 16InternetCopyright NotificationNo part may be reproduced except as authorized by written permission.The copyright and the foregoing restriction extend to reproduction in all media.© 2016, 3GPP Organizational Partners (ARIB, ATIS, CCSA, ETSI, TSDSI, TTA, TTC).All rights reserved.UMTS™ is a Trade Mark of ETSI registered for the benefit of its members3GPP™ is a Trade Mark of ETSI registered for the benefit of its Members and of the 3GPP Organizational PartnersLTE™ is a Trade Mark of ETSI currently being registered for the benefit of its Members and of the 3GPP Organizational Partners GSM® and the GSM logo are registered and owned by the GSM AssociationBluetooth® is a Trade Mark of the Bluetooth SIG registered for the benefit of its membersContentsForeword (18)1Scope (19)2References (19)3Definitions, symbols and abbreviations (22)3.1Definitions (22)3.2Abbreviations (24)4General (27)4.1Introduction (27)4.2Architecture (28)4.2.1UE states and state transitions including inter RAT (28)4.2.2Signalling radio bearers (29)4.3Services (30)4.3.1Services provided to upper layers (30)4.3.2Services expected from lower layers (30)4.4Functions (30)5Procedures (32)5.1General (32)5.1.1Introduction (32)5.1.2General requirements (32)5.2System information (33)5.2.1Introduction (33)5.2.1.1General (33)5.2.1.2Scheduling (34)5.2.1.2a Scheduling for NB-IoT (34)5.2.1.3System information validity and notification of changes (35)5.2.1.4Indication of ETWS notification (36)5.2.1.5Indication of CMAS notification (37)5.2.1.6Notification of EAB parameters change (37)5.2.1.7Access Barring parameters change in NB-IoT (37)5.2.2System information acquisition (38)5.2.2.1General (38)5.2.2.2Initiation (38)5.2.2.3System information required by the UE (38)5.2.2.4System information acquisition by the UE (39)5.2.2.5Essential system information missing (42)5.2.2.6Actions upon reception of the MasterInformationBlock message (42)5.2.2.7Actions upon reception of the SystemInformationBlockType1 message (42)5.2.2.8Actions upon reception of SystemInformation messages (44)5.2.2.9Actions upon reception of SystemInformationBlockType2 (44)5.2.2.10Actions upon reception of SystemInformationBlockType3 (45)5.2.2.11Actions upon reception of SystemInformationBlockType4 (45)5.2.2.12Actions upon reception of SystemInformationBlockType5 (45)5.2.2.13Actions upon reception of SystemInformationBlockType6 (45)5.2.2.14Actions upon reception of SystemInformationBlockType7 (45)5.2.2.15Actions upon reception of SystemInformationBlockType8 (45)5.2.2.16Actions upon reception of SystemInformationBlockType9 (46)5.2.2.17Actions upon reception of SystemInformationBlockType10 (46)5.2.2.18Actions upon reception of SystemInformationBlockType11 (46)5.2.2.19Actions upon reception of SystemInformationBlockType12 (47)5.2.2.20Actions upon reception of SystemInformationBlockType13 (48)5.2.2.21Actions upon reception of SystemInformationBlockType14 (48)5.2.2.22Actions upon reception of SystemInformationBlockType15 (48)5.2.2.23Actions upon reception of SystemInformationBlockType16 (48)5.2.2.24Actions upon reception of SystemInformationBlockType17 (48)5.2.2.25Actions upon reception of SystemInformationBlockType18 (48)5.2.2.26Actions upon reception of SystemInformationBlockType19 (49)5.2.3Acquisition of an SI message (49)5.2.3a Acquisition of an SI message by BL UE or UE in CE or a NB-IoT UE (50)5.3Connection control (50)5.3.1Introduction (50)5.3.1.1RRC connection control (50)5.3.1.2Security (52)5.3.1.2a RN security (53)5.3.1.3Connected mode mobility (53)5.3.1.4Connection control in NB-IoT (54)5.3.2Paging (55)5.3.2.1General (55)5.3.2.2Initiation (55)5.3.2.3Reception of the Paging message by the UE (55)5.3.3RRC connection establishment (56)5.3.3.1General (56)5.3.3.1a Conditions for establishing RRC Connection for sidelink communication/ discovery (58)5.3.3.2Initiation (59)5.3.3.3Actions related to transmission of RRCConnectionRequest message (63)5.3.3.3a Actions related to transmission of RRCConnectionResumeRequest message (64)5.3.3.4Reception of the RRCConnectionSetup by the UE (64)5.3.3.4a Reception of the RRCConnectionResume by the UE (66)5.3.3.5Cell re-selection while T300, T302, T303, T305, T306, or T308 is running (68)5.3.3.6T300 expiry (68)5.3.3.7T302, T303, T305, T306, or T308 expiry or stop (69)5.3.3.8Reception of the RRCConnectionReject by the UE (70)5.3.3.9Abortion of RRC connection establishment (71)5.3.3.10Handling of SSAC related parameters (71)5.3.3.11Access barring check (72)5.3.3.12EAB check (73)5.3.3.13Access barring check for ACDC (73)5.3.3.14Access Barring check for NB-IoT (74)5.3.4Initial security activation (75)5.3.4.1General (75)5.3.4.2Initiation (76)5.3.4.3Reception of the SecurityModeCommand by the UE (76)5.3.5RRC connection reconfiguration (77)5.3.5.1General (77)5.3.5.2Initiation (77)5.3.5.3Reception of an RRCConnectionReconfiguration not including the mobilityControlInfo by theUE (77)5.3.5.4Reception of an RRCConnectionReconfiguration including the mobilityControlInfo by the UE(handover) (79)5.3.5.5Reconfiguration failure (83)5.3.5.6T304 expiry (handover failure) (83)5.3.5.7Void (84)5.3.5.7a T307 expiry (SCG change failure) (84)5.3.5.8Radio Configuration involving full configuration option (84)5.3.6Counter check (86)5.3.6.1General (86)5.3.6.2Initiation (86)5.3.6.3Reception of the CounterCheck message by the UE (86)5.3.7RRC connection re-establishment (87)5.3.7.1General (87)5.3.7.2Initiation (87)5.3.7.3Actions following cell selection while T311 is running (88)5.3.7.4Actions related to transmission of RRCConnectionReestablishmentRequest message (89)5.3.7.5Reception of the RRCConnectionReestablishment by the UE (89)5.3.7.6T311 expiry (91)5.3.7.7T301 expiry or selected cell no longer suitable (91)5.3.7.8Reception of RRCConnectionReestablishmentReject by the UE (91)5.3.8RRC connection release (92)5.3.8.1General (92)5.3.8.2Initiation (92)5.3.8.3Reception of the RRCConnectionRelease by the UE (92)5.3.8.4T320 expiry (93)5.3.9RRC connection release requested by upper layers (93)5.3.9.1General (93)5.3.9.2Initiation (93)5.3.10Radio resource configuration (93)5.3.10.0General (93)5.3.10.1SRB addition/ modification (94)5.3.10.2DRB release (95)5.3.10.3DRB addition/ modification (95)5.3.10.3a1DC specific DRB addition or reconfiguration (96)5.3.10.3a2LWA specific DRB addition or reconfiguration (98)5.3.10.3a3LWIP specific DRB addition or reconfiguration (98)5.3.10.3a SCell release (99)5.3.10.3b SCell addition/ modification (99)5.3.10.3c PSCell addition or modification (99)5.3.10.4MAC main reconfiguration (99)5.3.10.5Semi-persistent scheduling reconfiguration (100)5.3.10.6Physical channel reconfiguration (100)5.3.10.7Radio Link Failure Timers and Constants reconfiguration (101)5.3.10.8Time domain measurement resource restriction for serving cell (101)5.3.10.9Other configuration (102)5.3.10.10SCG reconfiguration (103)5.3.10.11SCG dedicated resource configuration (104)5.3.10.12Reconfiguration SCG or split DRB by drb-ToAddModList (105)5.3.10.13Neighbour cell information reconfiguration (105)5.3.10.14Void (105)5.3.10.15Sidelink dedicated configuration (105)5.3.10.16T370 expiry (106)5.3.11Radio link failure related actions (107)5.3.11.1Detection of physical layer problems in RRC_CONNECTED (107)5.3.11.2Recovery of physical layer problems (107)5.3.11.3Detection of radio link failure (107)5.3.12UE actions upon leaving RRC_CONNECTED (109)5.3.13UE actions upon PUCCH/ SRS release request (110)5.3.14Proximity indication (110)5.3.14.1General (110)5.3.14.2Initiation (111)5.3.14.3Actions related to transmission of ProximityIndication message (111)5.3.15Void (111)5.4Inter-RAT mobility (111)5.4.1Introduction (111)5.4.2Handover to E-UTRA (112)5.4.2.1General (112)5.4.2.2Initiation (112)5.4.2.3Reception of the RRCConnectionReconfiguration by the UE (112)5.4.2.4Reconfiguration failure (114)5.4.2.5T304 expiry (handover to E-UTRA failure) (114)5.4.3Mobility from E-UTRA (114)5.4.3.1General (114)5.4.3.2Initiation (115)5.4.3.3Reception of the MobilityFromEUTRACommand by the UE (115)5.4.3.4Successful completion of the mobility from E-UTRA (116)5.4.3.5Mobility from E-UTRA failure (117)5.4.4Handover from E-UTRA preparation request (CDMA2000) (117)5.4.4.1General (117)5.4.4.2Initiation (118)5.4.4.3Reception of the HandoverFromEUTRAPreparationRequest by the UE (118)5.4.5UL handover preparation transfer (CDMA2000) (118)5.4.5.1General (118)5.4.5.2Initiation (118)5.4.5.3Actions related to transmission of the ULHandoverPreparationTransfer message (119)5.4.5.4Failure to deliver the ULHandoverPreparationTransfer message (119)5.4.6Inter-RAT cell change order to E-UTRAN (119)5.4.6.1General (119)5.4.6.2Initiation (119)5.4.6.3UE fails to complete an inter-RAT cell change order (119)5.5Measurements (120)5.5.1Introduction (120)5.5.2Measurement configuration (121)5.5.2.1General (121)5.5.2.2Measurement identity removal (122)5.5.2.2a Measurement identity autonomous removal (122)5.5.2.3Measurement identity addition/ modification (123)5.5.2.4Measurement object removal (124)5.5.2.5Measurement object addition/ modification (124)5.5.2.6Reporting configuration removal (126)5.5.2.7Reporting configuration addition/ modification (127)5.5.2.8Quantity configuration (127)5.5.2.9Measurement gap configuration (127)5.5.2.10Discovery signals measurement timing configuration (128)5.5.2.11RSSI measurement timing configuration (128)5.5.3Performing measurements (128)5.5.3.1General (128)5.5.3.2Layer 3 filtering (131)5.5.4Measurement report triggering (131)5.5.4.1General (131)5.5.4.2Event A1 (Serving becomes better than threshold) (135)5.5.4.3Event A2 (Serving becomes worse than threshold) (136)5.5.4.4Event A3 (Neighbour becomes offset better than PCell/ PSCell) (136)5.5.4.5Event A4 (Neighbour becomes better than threshold) (137)5.5.4.6Event A5 (PCell/ PSCell becomes worse than threshold1 and neighbour becomes better thanthreshold2) (138)5.5.4.6a Event A6 (Neighbour becomes offset better than SCell) (139)5.5.4.7Event B1 (Inter RAT neighbour becomes better than threshold) (139)5.5.4.8Event B2 (PCell becomes worse than threshold1 and inter RAT neighbour becomes better thanthreshold2) (140)5.5.4.9Event C1 (CSI-RS resource becomes better than threshold) (141)5.5.4.10Event C2 (CSI-RS resource becomes offset better than reference CSI-RS resource) (141)5.5.4.11Event W1 (WLAN becomes better than a threshold) (142)5.5.4.12Event W2 (All WLAN inside WLAN mobility set becomes worse than threshold1 and a WLANoutside WLAN mobility set becomes better than threshold2) (142)5.5.4.13Event W3 (All WLAN inside WLAN mobility set becomes worse than a threshold) (143)5.5.5Measurement reporting (144)5.5.6Measurement related actions (148)5.5.6.1Actions upon handover and re-establishment (148)5.5.6.2Speed dependant scaling of measurement related parameters (149)5.5.7Inter-frequency RSTD measurement indication (149)5.5.7.1General (149)5.5.7.2Initiation (150)5.5.7.3Actions related to transmission of InterFreqRSTDMeasurementIndication message (150)5.6Other (150)5.6.0General (150)5.6.1DL information transfer (151)5.6.1.1General (151)5.6.1.2Initiation (151)5.6.1.3Reception of the DLInformationTransfer by the UE (151)5.6.2UL information transfer (151)5.6.2.1General (151)5.6.2.2Initiation (151)5.6.2.3Actions related to transmission of ULInformationTransfer message (152)5.6.2.4Failure to deliver ULInformationTransfer message (152)5.6.3UE capability transfer (152)5.6.3.1General (152)5.6.3.2Initiation (153)5.6.3.3Reception of the UECapabilityEnquiry by the UE (153)5.6.4CSFB to 1x Parameter transfer (157)5.6.4.1General (157)5.6.4.2Initiation (157)5.6.4.3Actions related to transmission of CSFBParametersRequestCDMA2000 message (157)5.6.4.4Reception of the CSFBParametersResponseCDMA2000 message (157)5.6.5UE Information (158)5.6.5.1General (158)5.6.5.2Initiation (158)5.6.5.3Reception of the UEInformationRequest message (158)5.6.6 Logged Measurement Configuration (159)5.6.6.1General (159)5.6.6.2Initiation (160)5.6.6.3Reception of the LoggedMeasurementConfiguration by the UE (160)5.6.6.4T330 expiry (160)5.6.7 Release of Logged Measurement Configuration (160)5.6.7.1General (160)5.6.7.2Initiation (160)5.6.8 Measurements logging (161)5.6.8.1General (161)5.6.8.2Initiation (161)5.6.9In-device coexistence indication (163)5.6.9.1General (163)5.6.9.2Initiation (164)5.6.9.3Actions related to transmission of InDeviceCoexIndication message (164)5.6.10UE Assistance Information (165)5.6.10.1General (165)5.6.10.2Initiation (166)5.6.10.3Actions related to transmission of UEAssistanceInformation message (166)5.6.11 Mobility history information (166)5.6.11.1General (166)5.6.11.2Initiation (166)5.6.12RAN-assisted WLAN interworking (167)5.6.12.1General (167)5.6.12.2Dedicated WLAN offload configuration (167)5.6.12.3WLAN offload RAN evaluation (167)5.6.12.4T350 expiry or stop (167)5.6.12.5Cell selection/ re-selection while T350 is running (168)5.6.13SCG failure information (168)5.6.13.1General (168)5.6.13.2Initiation (168)5.6.13.3Actions related to transmission of SCGFailureInformation message (168)5.6.14LTE-WLAN Aggregation (169)5.6.14.1Introduction (169)5.6.14.2Reception of LWA configuration (169)5.6.14.3Release of LWA configuration (170)5.6.15WLAN connection management (170)5.6.15.1Introduction (170)5.6.15.2WLAN connection status reporting (170)5.6.15.2.1General (170)5.6.15.2.2Initiation (171)5.6.15.2.3Actions related to transmission of WLANConnectionStatusReport message (171)5.6.15.3T351 Expiry (WLAN connection attempt timeout) (171)5.6.15.4WLAN status monitoring (171)5.6.16RAN controlled LTE-WLAN interworking (172)5.6.16.1General (172)5.6.16.2WLAN traffic steering command (172)5.6.17LTE-WLAN aggregation with IPsec tunnel (173)5.6.17.1General (173)5.7Generic error handling (174)5.7.1General (174)5.7.2ASN.1 violation or encoding error (174)5.7.3Field set to a not comprehended value (174)5.7.4Mandatory field missing (174)5.7.5Not comprehended field (176)5.8MBMS (176)5.8.1Introduction (176)5.8.1.1General (176)5.8.1.2Scheduling (176)5.8.1.3MCCH information validity and notification of changes (176)5.8.2MCCH information acquisition (178)5.8.2.1General (178)5.8.2.2Initiation (178)5.8.2.3MCCH information acquisition by the UE (178)5.8.2.4Actions upon reception of the MBSFNAreaConfiguration message (178)5.8.2.5Actions upon reception of the MBMSCountingRequest message (179)5.8.3MBMS PTM radio bearer configuration (179)5.8.3.1General (179)5.8.3.2Initiation (179)5.8.3.3MRB establishment (179)5.8.3.4MRB release (179)5.8.4MBMS Counting Procedure (179)5.8.4.1General (179)5.8.4.2Initiation (180)5.8.4.3Reception of the MBMSCountingRequest message by the UE (180)5.8.5MBMS interest indication (181)5.8.5.1General (181)5.8.5.2Initiation (181)5.8.5.3Determine MBMS frequencies of interest (182)5.8.5.4Actions related to transmission of MBMSInterestIndication message (183)5.8a SC-PTM (183)5.8a.1Introduction (183)5.8a.1.1General (183)5.8a.1.2SC-MCCH scheduling (183)5.8a.1.3SC-MCCH information validity and notification of changes (183)5.8a.1.4Procedures (184)5.8a.2SC-MCCH information acquisition (184)5.8a.2.1General (184)5.8a.2.2Initiation (184)5.8a.2.3SC-MCCH information acquisition by the UE (184)5.8a.2.4Actions upon reception of the SCPTMConfiguration message (185)5.8a.3SC-PTM radio bearer configuration (185)5.8a.3.1General (185)5.8a.3.2Initiation (185)5.8a.3.3SC-MRB establishment (185)5.8a.3.4SC-MRB release (185)5.9RN procedures (186)5.9.1RN reconfiguration (186)5.9.1.1General (186)5.9.1.2Initiation (186)5.9.1.3Reception of the RNReconfiguration by the RN (186)5.10Sidelink (186)5.10.1Introduction (186)5.10.1a Conditions for sidelink communication operation (187)5.10.2Sidelink UE information (188)5.10.2.1General (188)5.10.2.2Initiation (189)5.10.2.3Actions related to transmission of SidelinkUEInformation message (193)5.10.3Sidelink communication monitoring (195)5.10.6Sidelink discovery announcement (198)5.10.6a Sidelink discovery announcement pool selection (201)5.10.6b Sidelink discovery announcement reference carrier selection (201)5.10.7Sidelink synchronisation information transmission (202)5.10.7.1General (202)5.10.7.2Initiation (203)5.10.7.3Transmission of SLSS (204)5.10.7.4Transmission of MasterInformationBlock-SL message (205)5.10.7.5Void (206)5.10.8Sidelink synchronisation reference (206)5.10.8.1General (206)5.10.8.2Selection and reselection of synchronisation reference UE (SyncRef UE) (206)5.10.9Sidelink common control information (207)5.10.9.1General (207)5.10.9.2Actions related to reception of MasterInformationBlock-SL message (207)5.10.10Sidelink relay UE operation (207)5.10.10.1General (207)5.10.10.2AS-conditions for relay related sidelink communication transmission by sidelink relay UE (207)5.10.10.3AS-conditions for relay PS related sidelink discovery transmission by sidelink relay UE (208)5.10.10.4Sidelink relay UE threshold conditions (208)5.10.11Sidelink remote UE operation (208)5.10.11.1General (208)5.10.11.2AS-conditions for relay related sidelink communication transmission by sidelink remote UE (208)5.10.11.3AS-conditions for relay PS related sidelink discovery transmission by sidelink remote UE (209)5.10.11.4Selection and reselection of sidelink relay UE (209)5.10.11.5Sidelink remote UE threshold conditions (210)6Protocol data units, formats and parameters (tabular & ASN.1) (210)6.1General (210)6.2RRC messages (212)6.2.1General message structure (212)–EUTRA-RRC-Definitions (212)–BCCH-BCH-Message (212)–BCCH-DL-SCH-Message (212)–BCCH-DL-SCH-Message-BR (213)–MCCH-Message (213)–PCCH-Message (213)–DL-CCCH-Message (214)–DL-DCCH-Message (214)–UL-CCCH-Message (214)–UL-DCCH-Message (215)–SC-MCCH-Message (215)6.2.2Message definitions (216)–CounterCheck (216)–CounterCheckResponse (217)–CSFBParametersRequestCDMA2000 (217)–CSFBParametersResponseCDMA2000 (218)–DLInformationTransfer (218)–HandoverFromEUTRAPreparationRequest (CDMA2000) (219)–InDeviceCoexIndication (220)–InterFreqRSTDMeasurementIndication (222)–LoggedMeasurementConfiguration (223)–MasterInformationBlock (225)–MBMSCountingRequest (226)–MBMSCountingResponse (226)–MBMSInterestIndication (227)–MBSFNAreaConfiguration (228)–MeasurementReport (228)–MobilityFromEUTRACommand (229)–Paging (232)–ProximityIndication (233)–RNReconfiguration (234)–RNReconfigurationComplete (234)–RRCConnectionReconfiguration (235)–RRCConnectionReconfigurationComplete (240)–RRCConnectionReestablishment (241)–RRCConnectionReestablishmentComplete (241)–RRCConnectionReestablishmentReject (242)–RRCConnectionReestablishmentRequest (243)–RRCConnectionReject (243)–RRCConnectionRelease (244)–RRCConnectionResume (248)–RRCConnectionResumeComplete (249)–RRCConnectionResumeRequest (250)–RRCConnectionRequest (250)–RRCConnectionSetup (251)–RRCConnectionSetupComplete (252)–SCGFailureInformation (253)–SCPTMConfiguration (254)–SecurityModeCommand (255)–SecurityModeComplete (255)–SecurityModeFailure (256)–SidelinkUEInformation (256)–SystemInformation (258)–SystemInformationBlockType1 (259)–UEAssistanceInformation (264)–UECapabilityEnquiry (265)–UECapabilityInformation (266)–UEInformationRequest (267)–UEInformationResponse (267)–ULHandoverPreparationTransfer (CDMA2000) (273)–ULInformationTransfer (274)–WLANConnectionStatusReport (274)6.3RRC information elements (275)6.3.1System information blocks (275)–SystemInformationBlockType2 (275)–SystemInformationBlockType3 (279)–SystemInformationBlockType4 (282)–SystemInformationBlockType5 (283)–SystemInformationBlockType6 (287)–SystemInformationBlockType7 (289)–SystemInformationBlockType8 (290)–SystemInformationBlockType9 (295)–SystemInformationBlockType10 (295)–SystemInformationBlockType11 (296)–SystemInformationBlockType12 (297)–SystemInformationBlockType13 (297)–SystemInformationBlockType14 (298)–SystemInformationBlockType15 (298)–SystemInformationBlockType16 (299)–SystemInformationBlockType17 (300)–SystemInformationBlockType18 (301)–SystemInformationBlockType19 (301)–SystemInformationBlockType20 (304)6.3.2Radio resource control information elements (304)–AntennaInfo (304)–AntennaInfoUL (306)–CQI-ReportConfig (307)–CQI-ReportPeriodicProcExtId (314)–CrossCarrierSchedulingConfig (314)–CSI-IM-Config (315)–CSI-IM-ConfigId (315)–CSI-RS-Config (317)–CSI-RS-ConfigEMIMO (318)–CSI-RS-ConfigNZP (319)–CSI-RS-ConfigNZPId (320)–CSI-RS-ConfigZP (321)–CSI-RS-ConfigZPId (321)–DMRS-Config (321)–DRB-Identity (322)–EPDCCH-Config (322)–EIMTA-MainConfig (324)–LogicalChannelConfig (325)–LWA-Configuration (326)–LWIP-Configuration (326)–RCLWI-Configuration (327)–MAC-MainConfig (327)–P-C-AndCBSR (332)–PDCCH-ConfigSCell (333)–PDCP-Config (334)–PDSCH-Config (337)–PDSCH-RE-MappingQCL-ConfigId (339)–PHICH-Config (339)–PhysicalConfigDedicated (339)–P-Max (344)–PRACH-Config (344)–PresenceAntennaPort1 (346)–PUCCH-Config (347)–PUSCH-Config (351)–RACH-ConfigCommon (355)–RACH-ConfigDedicated (357)–RadioResourceConfigCommon (358)–RadioResourceConfigDedicated (362)–RLC-Config (367)–RLF-TimersAndConstants (369)–RN-SubframeConfig (370)–SchedulingRequestConfig (371)–SoundingRS-UL-Config (372)–SPS-Config (375)–TDD-Config (376)–TimeAlignmentTimer (377)–TPC-PDCCH-Config (377)–TunnelConfigLWIP (378)–UplinkPowerControl (379)–WLAN-Id-List (382)–WLAN-MobilityConfig (382)6.3.3Security control information elements (382)–NextHopChainingCount (382)–SecurityAlgorithmConfig (383)–ShortMAC-I (383)6.3.4Mobility control information elements (383)–AdditionalSpectrumEmission (383)–ARFCN-ValueCDMA2000 (383)–ARFCN-ValueEUTRA (384)–ARFCN-ValueGERAN (384)–ARFCN-ValueUTRA (384)–BandclassCDMA2000 (384)–BandIndicatorGERAN (385)–CarrierFreqCDMA2000 (385)–CarrierFreqGERAN (385)–CellIndexList (387)–CellReselectionPriority (387)–CellSelectionInfoCE (387)–CellReselectionSubPriority (388)–CSFB-RegistrationParam1XRTT (388)–CellGlobalIdEUTRA (389)–CellGlobalIdUTRA (389)–CellGlobalIdGERAN (390)–CellGlobalIdCDMA2000 (390)–CellSelectionInfoNFreq (391)–CSG-Identity (391)–FreqBandIndicator (391)–MobilityControlInfo (391)–MobilityParametersCDMA2000 (1xRTT) (393)–MobilityStateParameters (394)–MultiBandInfoList (394)–NS-PmaxList (394)–PhysCellId (395)–PhysCellIdRange (395)–PhysCellIdRangeUTRA-FDDList (395)–PhysCellIdCDMA2000 (396)–PhysCellIdGERAN (396)–PhysCellIdUTRA-FDD (396)–PhysCellIdUTRA-TDD (396)–PLMN-Identity (397)–PLMN-IdentityList3 (397)–PreRegistrationInfoHRPD (397)–Q-QualMin (398)–Q-RxLevMin (398)–Q-OffsetRange (398)–Q-OffsetRangeInterRAT (399)–ReselectionThreshold (399)–ReselectionThresholdQ (399)–SCellIndex (399)–ServCellIndex (400)–SpeedStateScaleFactors (400)–SystemInfoListGERAN (400)–SystemTimeInfoCDMA2000 (401)–TrackingAreaCode (401)–T-Reselection (402)–T-ReselectionEUTRA-CE (402)6.3.5Measurement information elements (402)–AllowedMeasBandwidth (402)–CSI-RSRP-Range (402)–Hysteresis (402)–LocationInfo (403)–MBSFN-RSRQ-Range (403)–MeasConfig (404)–MeasDS-Config (405)–MeasGapConfig (406)–MeasId (407)–MeasIdToAddModList (407)–MeasObjectCDMA2000 (408)–MeasObjectEUTRA (408)–MeasObjectGERAN (412)–MeasObjectId (412)–MeasObjectToAddModList (412)–MeasObjectUTRA (413)–ReportConfigEUTRA (422)–ReportConfigId (425)–ReportConfigInterRAT (425)–ReportConfigToAddModList (428)–ReportInterval (429)–RSRP-Range (429)–RSRQ-Range (430)–RSRQ-Type (430)–RS-SINR-Range (430)–RSSI-Range-r13 (431)–TimeToTrigger (431)–UL-DelayConfig (431)–WLAN-CarrierInfo (431)–WLAN-RSSI-Range (432)–WLAN-Status (432)6.3.6Other information elements (433)–AbsoluteTimeInfo (433)–AreaConfiguration (433)–C-RNTI (433)–DedicatedInfoCDMA2000 (434)–DedicatedInfoNAS (434)–FilterCoefficient (434)–LoggingDuration (434)–LoggingInterval (435)–MeasSubframePattern (435)–MMEC (435)–NeighCellConfig (435)–OtherConfig (436)–RAND-CDMA2000 (1xRTT) (437)–RAT-Type (437)–ResumeIdentity (437)–RRC-TransactionIdentifier (438)–S-TMSI (438)–TraceReference (438)–UE-CapabilityRAT-ContainerList (438)–UE-EUTRA-Capability (439)–UE-RadioPagingInfo (469)–UE-TimersAndConstants (469)–VisitedCellInfoList (470)–WLAN-OffloadConfig (470)6.3.7MBMS information elements (472)–MBMS-NotificationConfig (472)–MBMS-ServiceList (473)–MBSFN-AreaId (473)–MBSFN-AreaInfoList (473)–MBSFN-SubframeConfig (474)–PMCH-InfoList (475)6.3.7a SC-PTM information elements (476)–SC-MTCH-InfoList (476)–SCPTM-NeighbourCellList (478)6.3.8Sidelink information elements (478)–SL-CommConfig (478)–SL-CommResourcePool (479)–SL-CP-Len (480)–SL-DiscConfig (481)–SL-DiscResourcePool (483)–SL-DiscTxPowerInfo (485)–SL-GapConfig (485)。
新视野英语教程第三版2UNIT2TrendsandFads知识讲解
掌上游戏机 handheld game console
Warmingup
Exercises
Around the Topic
Section A
Section B
Section C
Our Changing Lifestyle: Trends and Fads
These days, lifestyles have a tendency to change so fast. It is more than just clothing and hairstyles that are in style one year and out of date the next; it’s a whole way of living.
Return
Leading in
Exploring the Topic
Around the Topic Section A
Section B
Section C
Suggested answer:
When it comes to the typical fashionable Items possessed by the college students today, so far as I know, the following things are worth mentioning. They are computer (both for learning and games), Mobile phone (for communication) and MP3 (both for learning and entertaining).
one-piece dress Chinese tunic suit liberation shoes overalls; dungarees; jeans the flared trousers; the bell-bottoms a sailor’s striped shirt goggles
ALFVéNIC HEATING OF ACCRETION DISKS
A s t r o p h y s i c a l P l a s m a s : C o d e s , M o d e l s , a n d O b s e r v a t i o n s (M e x i c o C i t y , 25-29 O c t o b e r 1999)E d i t o r s : J a n e A r t h u r , N a n c yB r i c k h o u s e , & J o s é F r a n c o RevMexAA (Serie de Conferencias),9,103–104(2000)ALFV ´ENIC HEATING OF ACCRETION DISKSM.J.Vasconcelos,V.Jatenco-Pereira,and R.OpherInstituto Astronˆo mico e Geof´ısico,Universidade de S˜a o Paulo,BrasilRESUMENInvestigamos los efectos del calentamiento generado por la disipaci´o n tur-bulenta y nolineal de ondas de Alfv´e n.Nuestros resultados dependen de dospar´a metros:f =δv/v A ,que es una medida del nivel de turbulencia y F = /Ωique es la frecuencia promedio de las ondas (δv ,v A y son la amplitud,velocidad yfrequencia de las ondas de Alfv´e n y Ωi es la frecuencia ciclotr´o n de los iones).S´o lose estudia una fracci´o n peque˜n a del disco,de 0.1AU a parado con elcalentamiento de la disipaci´o n viscosa,encontramos que el calentamiento Alfv´e nicoes importante para R > temperatura aumenta,aumentando el grado deionizaci´o n del sistema.El incremento de temperatura es mayor cuando se incluye laradiaci´o n de la estrella influencia de la inestabilidad magnetorotacionalse extiende a una mayor parte del disco debido al calentamiento Alfv´e nico.ABSTRACTIn this work,we investigate the effects of heating generated by nonlinear andturbulent damping of Alfv´e n waves.Our results are a function of two parameters:f =δv/v A ,which is a measure of the degree of turbulence,and F = /Ωi ,which isthe average frequency of the waves (δv ,v A and are the amplitude,velocity andfrequency of the Alfv´e n waves,respectively,and Ωi is the ion cyclotron frequency).Only a small portion of the disk is studied,ranging from 0.1AU to 1.4AU.Wefind that,when compared with the heating generated by viscous dissipation,theAlfv´e nic heating is important for R >0.5AU.An increase in temperature occurs,which causes an increase in the degree of ionization of the system.When irradiationfrom the central star is taken into account the increase in temperature is muchmore significant.Due to Alfv´e nic heating,the influence of the magnetorotationalinstability extends to a greater part of the protostellar accretion disk.Key Words:ACCRETION DISKS —MHD —STARS:PRE-MAIN SE-QUENCE —W A VES1.ALFV ´ENIC HEATINGIn this work,we study two damping mechanisms of Alfv´e n waves,both nonlinear and turbulent.In nonlinear damping,waves of great amplitude interact to create magnetosonic waves,which are easily damped.Energy from the waves is thus transfered to the medium as thermal energy.The turbulent damping proceeds as a cascade of energy from large to small scale,where microscopic processes dissipate the energy of the wave.We assume that Alfv´e nic heating is an additional source of energy,acting together with viscous dissipation.In order to evaluate the energy transfered by the damping process,we need to know the damping length or the rate of damping.A more comprehensive derivation of the following equations can be found in Vasconcelos,Jatenco-Pereira,&Opher (2000).The energy dissipated by the nonlinear and turbulent damping of Alfv´e n waves is given byD NL =√4f 4F eξµ 1/2 H 0(ρT )1/2B 2dz ,(1)103A s t r o p h y s i c a l P l a s m a s : C o d e s , M o d e l s , a n d O b s e r v a t i o n s (M e x i c o C i t y , 25-29 O c t o b e r 1999)E d i t o r s : J a n e A r t h u r , N a n c yB r i c k h o u s e , & J o s é F r a n c o 104VASCONCELOS,JATENCO-PEREIRA,&OPHERD T = f4π 32 H 0B 7/2ρ−1/2dz ,(2)where e is the electric charge,ξis a constant,m i is the ion mass,c is the velocity of light,γis the adiabatic coefficient, is the gas constant,µis the mean molecular weight,ρis the density,T is temperature and B is the magnetic field,assumed to be vertical and uniform.We study three different situations in two disk models:1)the standard,optically thick,geometrically thin,stationary accretion disk,and 2)the layered model disk of Gammie (1996).The different profiles considered are:i)constant density and temperature,ii)varying density (ρ=ρ0exp(−z/H ))and constant temperature,iii)varying density (ρ=ρ0exp(−z/H ))and temperature (T =T 0exp(−z/H )).2.RESULTS AND DISCUSSION Nonlinear Alfv´e nic heating is found to be more important than viscous dissipation in the outer part of the disk region considered (R >0.5AU).For all profiles the Alfv´e nic energy dissipation is greater than viscous dissipation.Irradiation by the central star is very important for all radii and if we have nonlinear Alfv´e nic heating and irradiation acting at the same time in the disk,the increase in temperature is significant.Temperatures obtained with Alfv´e nic dissipation in the model of the layered disk are the highest,for R >0.2AU.The energies deposited by turbulent damping of Alfv´e n waves are very high,as compared with viscous energy.Dissipation of turbulent energy is important for all radii considered,even when irradiation is taken into account.M.J.V.would like to thank the Brazilian agency FAPESP for financial support.V.J.P.and R.O.acknowledge the Brazilian agencies FAPESP and CNPq for partial support.We also would like to acknowledge the project PRONEX (No.41.96.0908.00)for partial support.REFERENCES Gammie,C.F.1996,ApJ,457,355Vasconcelos,M.J.,Jatenco-Pereira,V.,&Opher,R.2000,ApJ,submittedM.J.Vasconcelos,V.Jatenco-Pereira,and R.Opher:Instituto Astronˆo mico e Geof´ısico,Universidade de S˜a o Paulo,Av.Miguel St´e fano 4200,S˜a o Paulo,S.P.04301-904,Brasil (jaque,jatenco,opher@p.br).。
光谱层英文版
光谱层英文版The Spectral Layer: Unveiling the Invisible RealmThe universe we inhabit is a tapestry of intricately woven elements, each thread contributing to the grand tapestry of existence. Amidst this intricate web, lies a realm that is often overlooked, yet holds the key to unlocking the mysteries of our reality. This realm is the spectral layer – a realm that transcends the boundaries of our visible world and delves into the unseen realms of energy and vibration.At the heart of the spectral layer lies the electromagnetic spectrum –a vast and diverse range of wavelengths and frequencies that encompass the entirety of our physical world. From the low-frequency radio waves to the high-energy gamma rays, the electromagnetic spectrum is the foundation upon which our understanding of the universe is built. It is within this spectrum that we find the familiar visible light, the spectrum of colors that we perceive with our eyes, but it is only a small fraction of the vast and diverse tapestry that makes up the spectral layer.Beyond the visible spectrum, there lies a realm of unseen energies that are integral to the very fabric of our existence. Infrared radiation, for instance, is a form of electromagnetic radiation that is invisible to the human eye but plays a crucial role in the transfer of heat and the functioning of various biological processes. Similarly, ultraviolet radiation, though invisible to us, is essential for the production of vitamin D and the regulation of circadian rhythms.But the spectral layer extends far beyond the confines of the electromagnetic spectrum. It is a realm that encompasses the vibrations and frequencies of all matter and energy, from the subatomic particles that make up the building blocks of our universe to the vast cosmic structures that span the vastness of space. These vibrations and frequencies, though often imperceptible to our senses, are the foundation upon which the entire universe is built.At the quantum level, the spectral layer reveals the true nature of reality. Subatomic particles, such as electrons and quarks, are not merely static entities but rather dynamic oscillations of energy, each with its own unique frequency and vibration. These vibrations, in turn, give rise to the fundamental forces that govern the behavior of matter and energy, from the strong nuclear force that holds the nucleus of an atom together to the mysterious dark energy that drives the expansion of the universe.But the spectral layer is not merely a realm of the infinitely small. It also encompasses the vast and expansive structures of the cosmos, from the intricate patterns of galaxies to the pulsing rhythms of celestial bodies. The stars that dot the night sky, for instance, are not merely points of light but rather vast nuclear furnaces, each emitting a unique spectrum of electromagnetic radiation that can be detected and analyzed by scientists.Through the study of the spectral layer, we have gained unprecedented insights into the nature of our universe. By analyzing the spectra of distant galaxies, for example, we can determine their chemical composition, their age, and even their rate of expansion –information that is crucial for our understanding of the origins and evolution of the cosmos.But the spectral layer is not just a realm of scientific inquiry – it is also a realm of profound spiritual and metaphysical exploration. Many ancient and indigenous cultures have long recognized the importance of the unseen realms of energy and vibration, and have developed sophisticated systems of understanding and interacting with these realms.In the traditions of Hinduism and Buddhism, for instance, the concept of the chakras – the seven energy centers that are believed to govern various aspects of our physical, emotional, and spiritualwell-being – is a manifestation of the spectral layer. These energy centers are believed to be connected to specific frequencies and vibrations, and the practice of chakra meditation and balancing is seen as a way to align oneself with the natural rhythms of the universe.Similarly, in the traditions of shamanism and indigenous healing practices, the concept of the "spirit world" or the "unseen realm" is closely tied to the spectral layer. Shamans and healers are often said to be able to perceive and interact with the unseen energies that permeate our world, using techniques such as drumming, chanting, and plant medicine to access these realms and bring about healing and transformation.In the modern era, the spectral layer has become the subject of intense scientific and technological exploration. From the development of advanced imaging technologies that can reveal the unseen structures of the human body to the creation of sophisticated communication systems that harness the power of the electromagnetic spectrum, the spectral layer has become an essential component of our understanding and manipulation of the physical world.Yet, despite the immense progress we have made in our understanding of the spectral layer, there is still much that remainsunknown and mysterious. The nature of dark matter and dark energy, for instance, remains one of the greatest unsolved puzzles in modern physics, and the true nature of consciousness and the relationship between the physical and the metaphysical realms continues to be a subject of intense debate and exploration.As we continue to delve deeper into the spectral layer, we may uncover even more profound insights into the nature of our reality. Perhaps we will discover new forms of energy and vibration that have yet to be detected, or perhaps we will find that the boundaries between the seen and the unseen are far more permeable than we ever imagined. Whatever the future may hold, one thing is certain: the spectral layer will continue to be a source of fascination, inspiration, and mystery for generations to come.。
医学英语词汇（S2）_医学英语词汇
speak 说，讲，陈述speaker 扬声器，话筒，喇叭speaking tube 传音筒spear drill 矛状锥，剑尖锥spear point drill 剑尖锥spear poing flat drill 剑尖平锥spec. (1.specification 2.specimen) ①说明书②标本special ①特殊的，专门的②专刊special accessories 专用附件special digital computer 专用计算机special effect generator 特技效果发生器specialist 专家speciality 特点，专业specialize 专门化，特殊化，限定special licence 特别许可证special procedure equipment 特殊程序设备special purpose computer 专用计算机species 种类specific 特有的，专门的，比（的）specific activity 比活性specification (abbr. spec.) ①说明书②规格，规范specific density 比重specific gravity (abbr. sp. gr.) 比重specific gravity balance 比重天平specific gravity bottle 比重瓶specific heat 比热specific ion electrode 离子选择电极specificity 特异性，专一性specific ratio 比率specific resistance 电阻率，比电阻specific value 比值specific volume 比容specific weight 比重specify ①规定，指定②详细说明specillum 探子，探杆specimen 标本，样品specimen bottle 样本瓶specimen copy 样本specimen disc 样品盘specimen holder 标本夹specimen jar 标本缸specimen trap 标本收集器specimen trimmer 标本粗割机specimen vial 标本管形瓶spectacles 眼镜，平光眼镜spectral 光谱，频谱的spectral lamp 光谱灯spectral line 光谱线spectral phonoangiography 光谱血管音描记术spectral phonocardiogram 光谱心音图spectral phonocardiograph 光谱心音描记器spectro- 光谱，分光spectrochrome 色光谱的spectrocolorimeter ①分光比色计②单色盲分光镜spectrocolorimetry 光谱色度学spectrocomparator 光谱比较仪spectrofluorimeter 荧光分光计spectrofluorometer 荧光分光计spectrofluorometry 荧光光谱测定法spectrofluorophotometer 荧光分光光度计spectrogram 光谱图spectrogrph 摄谱仪，光谱仪spectrographic camera 光谱照像机spectrography 摄谱术spectrometer 分光计，光谱计spectrometry 分光术，光谱测定法spectromicroscope 分光显微镜spectromonitor 分光监视器spectrophotometer 分光光度计，分光比色计spectrophotometer cell 分光光度计比色皿spectrophotometry 分光光度测定法spectropolarimeter 分光偏振计，旋光分光计spectropyrheliometer 日射光谱仪spectroradiometer 分光辐射谱仪spectroscope 分光镜，分光仪spectroscopy 分光镜检查spectrum 光谱，光系，谱specular image 镜像speculum ①窥器，张开器②窥镜speculum forceps 窥器钳speech 语言，演说speech amplifier 音频放大器speech coder 语言编码器speech recognizing machine 语言识别机speed 速率，速度，转数speed autoclave 快速灭菌器speedometer 示速器，里程计spermatangium 精子器spf (spectrophotofluorometer) 荧光分光光度计sp. gr. (specific gravity) 比重spheno- 楔形，蝶骨sphenoidal rasp 蝶骨锉sphenoid sinus canula 蝶窦套管sphenoid sinus curette 蝶窦刮匙sphenoid sinus rongeur 鼻蝶窦咬骨钳sphenometer （楔形）骨片测量器sphenotribe 碎颅器sphere 球体，区域，范围，界sphere introducer 眼球置入器spherical aberration 球面像差spherical lens 球面镜片spherical projection perimeter 球形投影视野计spherocylinder 球柱透镜spheroid ①球形的②球形体spherometer 球径计sphincter 括约肌sphincteroscope 肛门括约肌镜sphincteroscopy 肛门括约肌匀检查sphincterotome 括约肌切开器sphygmo- 脉，脉搏sphygmobologram 脉能图，胸压曲线sphygmobolograph 脉能描记器sphygmobolometer 脉能描记器，脉压计sphygmobolometry 脉能描记法，脉压测量术sphygmocardiogram 脉搏心动图sphygmocardiograph 脉搏心动描记器sphygmocardioscope 脉搏心音描记器sphygmochronograph 脉搏自动描记器sphygmochronography 脉搏自动描记法sphygmodynamometer 脉搏力计sphygmodynamometry 脉搏测量法sphygmogram 脉搏图，脉搏曲线sphygmograph 脉搏描记器，脉搏计sphygmograph transducer 脉搏计换能器sphygmography 脉搏描记法sphygmoid 脉样的，脉搏状的sphygmology 脉学，脉搏学sphygmomanometer 血压计sphygmomanometroscope 复式血压计sphygmomanometry 血压测量法sphygmometer 脉搏计sphygmometrograph 血压描记器(记录最高和最低动脉血压)sphygmometroscope 听脉血压计，听力测压器sphygmo-oscillometer 示波血压计，振动血压计sphygmopalpation 按脉（法），切脉（法）sphygmophone 脉音听诊器sphygmoplethysmogrph 脉搏体积描记器，脉搏容积计sphygmoscope 脉搏检视器，脉镜sphygmoscopy 脉搏检查sphygmosignal 脉（搏振）辐检视器，脉搏信号器sphygmosystole 收缩期脉搏曲线sphygmotachograph 血流速度描记器sphygmotachymeter 脉搏速度计sphygmotonogram 血压脉搏图skphygmotonograph 血压脉搏描记器，脉动力描记器sphygmotonometer ①脉动力计，动脉管壁弹力计②眼底血压计sphygmous 脉搏的sphygmoviscosimetry 血压血液粘度测量法spica 穗形绷带，人字形绷带spider ①蜘蛛②三脚架，支座spider- web antenna 蛛网天线spigot ①插口，插销②龙头spike ①钉②脉冲，波峰（示波图）spike potential 峰电位spinal bone plate 脊柱接骨板spinal cord 脊髓spinal forceps 脊柱钳spinal fusion curette 脊柱凑合术刮匙spinal fusion osteotome 脊凑合术骨凿spinal fusion plate 脊柱接合板spinal manometer 脊椎测压计spinal marrow 骨髓spinal needle 脊椎穿刺针spinal retractor 脊柱牵开器spinal rongeur 棘突咬骨钳spinal screw 脊柱螺钉spinal support 脊柱支持器spinawl 破皮锥，破皮钻spine ①脊柱②棘，刺spine chisel 脊柱凿spine saw 脊柱锯spinner 旋转器spinogram ①脊柱x射线（照）片②脊髓造影照片spinthariscope 闪烁镜spintherometer x射线透度计spintometer x射线透度计spiral ①螺旋的②螺旋管③螺旋钻spiral agitator 螺旋式搅拌器spiral drill 螺丝钻头spiral separator 螺旋分离器spirit 酒精，醑剂spirit blowtorch 酒精喷灯spirit gauge 酒精比重计spirit lamp 酒精灯spirit thermometer 酒精温度计spiro- 呼吸spiroanalyzer 呼吸功能分析器spirocomputer 呼吸功能计算器spirogram 呼吸（描记）图spirograph 呼吸量描记器，肺功能测定仪spirography 呼吸描记法spiroid 螺旋样的spiro-index 呼吸指数spirometer 呼吸量计，呼吸气量测定器spirometer alarm 呼吸量计报警器spirometric 肺量测定的spirometry 肺量测定法，呼吸量测定法spirophore 柜式人工呼吸器spiropulsator 吸入麻醉器spiroscope 呼吸量测视器spiroscopy 呼吸量测视法spittoon 痰盂splanchna 内脏splanchnic retractor 内脏牵开器splanchno- 内脏splanchnoscopy 内窥镜检查splanchnotribe 夹肠器spleen 脾spleen pedicle clamp 脾蒂钳splenic venography 脾门静脉造影术spleno- 脾splenogram 脾x射线照片splenography 脾 x射线照像术splenoportography 脾门静脉x射线造影术splice ①缝接②加板splint 夹板，夹splint and bandage 夹板绷带splinter 裂片，碎片屑splinter forceps 取裂片镊splint of wood 木夹板split antenna 隙缝天线split stream inyector 分流注射器splitter ①分裂器②分离器③分流器splitting chisel 裂片凿splitting forceps 分劈钳splitting instrument 分解器split ventricular trocar 裂隙室套管spokeshave 鼻用环形刀sponge 海绵sponge biopsy 棉拭活组织检查sponge bowl 海绵碗sponge dressing forceps 弹性敷料镊sponge forceps 海绵钳sponge holder 海绵夹，持绵器sponge holding forceps 海绵夹持钳，持海绵钳sponge probang 海绵除鲠器sponge tent 海绵塞条spongia 海绵sponsor ①发起人，资助人②发起，主办spontaneous 任意的，自发的spontaneous brain wave 自发性脑电波spool 线圈，卷盘spoon 匙spoonful 匙，一匙量spoon knife 匙型刀spoon shaped clamp 匙型夹spoon shaped speculum 匙形窥器spoon type anastomosis forceps 匙型吻合钳spot 斑，光点，部位spot film device x射线点片器spot film radiography 适时x射线照像术spot film roentgenography 适时x射线照像术spotlight 聚光灯，反光灯spotlighting illuminator 焦点照明器spot paper 点滴反应用滤纸spout 喷嘴，槽spray ①喷雾器，喷嘴②喷雾剂spray bottle 喷雾瓶spray bottle heater 喷雾瓶加热器spray bottle nozzle 喷雾瓶嘴spray bottle warmer 喷雾瓶加温器spray dryerin lab 实验室喷雾干燥器sprayer ①喷雾器②喷嘴spray jet 喷雾器spray nozzle 喷嘴spray pistol 喷雾枪spreader 摊开器，扩张器spreading forceps 扩张钳spring ①弹簧②弹性spring balance 弹簧天平，弹簧称spring bending pliers 曲簧钳spring forceps 弹簧钳spring guide 弹簧导子srs x-knife(stereotactil radiosuryerysystem) 立体定位放射外科系统（简称x刀）srt 多向立体定位放射疗法spring knife 弹簧刀spring kymograph 弹簧记波器spring lancet ①弹簧刀②弹簧刺血针spring manometer 弹簧测压计spring mattress 弹簧褥子spring phlebotome 弹簧静脉刀spring scarificator 弹簧划痕器spring socket 弹簧插座spring washer 弹簧垫圈spring wire 弹簧丝sprue former 铸道形成针spud 铲，剥皮刀spur crusher 骨刺压碎器spurious 假的，伪造的spurt 喷出，喷射sputum 痰sputum bottle 痰瓶sputum cup 痰杯sputum tube 容痰管square 正方形，平方squared paper 方格纸square punch 方型钻孔器square shaped 方型的square tray anth cap 有盖方盘squeeze 压缩，挤sqyeeze dtbanineter 手握力计squeezer 压榨器squeezing forceps 砂眼压榨镊squid 超导量子干涉仪squint hook 斜视钩squint knife 斜视刀sr (strontium) 锶srs 立体安位射线外科sseg (segmental spinal electrogram) 节段性脊电图stab ①刺②杆squid (superconduction quantum interference device) 超导量子干涉仪（测量心磁脑磁信息）stabber 锥，穿索针stability 稳定性stabilivolt 稳压管stabilization 稳定stabilizator ①稳压器②稳定器stabilizer ①稳压器②固位器，稳定器stabilograph 稳定性测定器stabilovolt tube 稳压管stab knife 穿刺刀stable tracer isotope 稳定示踪同位素stack ①堆积，叠②捆，束，组，套stacked antenna 多层天线stacker ①可升降摄像机台②叠式存储器stactometer 测滴计，滴量计stadia computer 视距计算器stadiometer 测距仪staff ①探杆，导引探子②杆stage （显微镜）载物台，镜台stage micrometer 镜台测微器（显微镜）stagonometer （表面张力）滴重计stain 着色剂，染料stained preparation 染色标本stainer 染色器staining 染色，染色法staining bottle 染色瓶staining dish 染色皿staining jax 染色缸staining machine 染色机staining technique 染色技术stainless 不锈的，不锈钢的stainless steel 不锈钢=yustlessstcel stainless steel silk 不锈钢丝stainless steel wire 不锈钢丝stain smear 染色涂片stalagmometer 表面张力滴定计，滴数计stall 手指护套stalloy 硅钢片stamp ①图章②盖印，标出③邮票stand 台，座，支架standard (abbr.std.) 标准，规格，样品standard accessory 标准附件standard candle 标准烛光standard cell 标准电池standard curve 标准曲线standard deviation 标准偏差standard electrode 标准电极standard emitron 光电摄像管standard error (abbr.s.e.) 标准误差standardizition 标准化，标定法standard lead 标准导程standard lens 标准镜头standard rocking microtome 标准摇动式切片机standard set-up 标准装置standard solution 标准溶液standard specifications 标准规格standard technique 标准技术，标准法standard volume 标准容积（理想气体在标准温度和压力下的体积，即=22.414公升）stand-by ①备用品②准备standing ①放置②固定的，直立的stand magnet 立式吸铁器standpoint 立场，观点stannum (abbr.sn) 锡staphylagra 悬雍垂钳staphyle 悬雍垂staphylo- 悬雍垂staphylorrhaphy elevator 软腭缝合用起子staphylotome 悬雍垂切除刀staple ①u形钉，肘钉②钉书钉staple driver 骨科u形钉起子stapler ①小钉书机②中药袋封口机star 星，星形物starch 淀粉starch-sugar 糊精star connection 星形联接start 起动，开始starter 起动器，发射器stasimetry 稠度测量法stat. 镭射气单位（计算镭放射量的单位相当于0.364毫居里）state ①状态，情况②叙述，说明statement 声明，报告书statement of claims 索赔清单static ①静电的②固定的static campimeter 静态平面视野计，中心量光觉视野计static electrical apparatus 间动电疗机static electricity 静电static electrometer 静电计static probe 固定探头（b超）statics ①静电学②静电干扰station 电台，站，地点stationary grid 静止滤线栅statistical distribution 统计分布statistics 统计学statometer 眼球突出计statoscope 自记微气压计，微动气压计status 状况，地位stay suture clamp 支座缝合夹std. atm. (standard atmosphere) 标准大气压steadiness apparatus 共济失调描记器steady 稳定的，均匀的steam 蒸汽，汽steam autoclave 蒸汽灭菌器steam disinfecting apparatus 蒸汽消毒器steam disinfector 蒸汽消毒器steam gage 汽压计，蒸汽压力表steam inhalar apparatus 蒸汽吸入器steam inhaler 蒸汽吸入器steam kettle 蒸汽锅steam piston 蒸汽活塞steam pressure gauge 蒸汽压力表steam pressure respirator 蒸汽加压呼吸器steam sterilization 蒸汽灭菌法steam sterilizer 蒸汽灭菌器steam under pressure 加压蒸汽steam vapor cabinet 蒸汽浴箱steam vaporiser 蒸汽喷雾器steel 钢steel bending wire 钢曲丝steel bur 钢钻steel measure tape 钢卷尺steel rule 钢尺steel spoon 钢匙steel strip 钢条steel tape 钢卷尺steel thimble 钢套管steel wire 钢丝steering 操纵，控制stellite 钨铬钴合金stem 柄，杆，把stem-pessary 有杆子宫托stencil ①模绘板②蜡纸stender dish 施滕德氏皿（组织标本制备及染色的大小形状不同的器皿）stenocompressor 腮腺管压闭器stenopaic spectacles 小孔镜stenosis 狭窄step ①极，档，阶梯②间歇式的step-down transformer 降压器step lens 棱镜stepless 连续的，均匀的step-penetrameter 楔形梯级式x射线透度计step-up 升高，加快step-up transformer 升压器step-wedge 楔形梯级step-wedge penetrameter 楔形梯级式x射线透度计steradian 球面度（立体角单位）stere 千升，立方米（容量单位）stereo ①立体，实体②立体镜③立体照片stereo- 立体，实体stereo-amplifier 立体声放大器stereobinocular microscope 立体双目显微镜stereo-camera 立体摄像机stereocampimeter 立体视野计stereocardiography 空间心电向量描记法stereo-cinefluorography 立体荧光电影摄像术stereo effect 立体声效应stereoencephaloscope 立体窥脑器，脑检视仪stereoencephalotome 立体脑切开器，脑定点切开器stereoencephalotomy 脑定点切开术stereofluoroscopy 立体荧光屏透视检查stereogram 立体照片，立体x射线照片stereograph 立体照片，立体x射线照片stereography 立体x射线照像术stereoisomer 立体异构体stereoisomerism 立体异构stereo-magnifier 立体放大镜stereometer ①体积计②比重计stereometry ①体积测定法②比重测定法stereomicrography 立体显微摄影stereomicroscope 实体显微镜，体视显微镜stereomodel 立体模型stereomonoscope 双眼单体镜stereo-movie 立体电影stereo-ophthalmoscope 双目检眼镜，立体检眼镜stereo-orthoptor 视轴矫正实体镜，体视矫正器stereophantoscope 体视绘图器stereophenomenon 体视现象stereophonic broadcast 立体声广播stereophony 立体声stereophorometer 立体隐斜视矫正器stereophoroscope 活动影片检视器stereophotogrammetry 立体照像测量术stereophotograph 立体照片stereophotography 立体摄影，立体照像术stereophotomicrograph 立体显微照片stereoplotter 立体绘图仪stereopter 实体视力检查器stereopticon ①幻灯②幻灯机，投影放大器stereoradiographic unit 立体摄影装置stereoradiography 实体x射线照像术stereo receiver 立体声收音机stereo recorder 立体声录音机stereo reflex camera 立体反射线照像机stereoroentgenograph 立体x射线照片stereoroentgenoscopy 立体x 线透视检查stereoscan photograph 扫描电镜照片stereoscope 立体镜，体视镜stereoscope picture 立体照片stereoscopic 立体的，体视的stereoscopic camera 立体照像机stereoscopic film 立体电影，立体影片stereoscopic fluoroscopy 实体荧光屏透视检查stereoscopic image 立体影像stereoscopic microscope 立体显微镜stereoscopic radiograph 立体x射线照片stereoscopic television 立体电视stereoscopic zoom microscope 体视变焦显微镜stereoscopy 实体镜检查法stereoskiagraphy 立体x射线照像术stereostroboscope 立体动态镜，体视频闪观测器stereotactic 立体定位的stereo tape 立体声录音带stereotactic rodiosurgery srstem(srs) 立体立位放射手术系统（简称x-xnife）stereotaxic apparatus 立体定位仪stereotelevision 立体电视stereo viewer 立体观片灯sterilamp 灭菌灯sterile 灭菌的，消毒的sterile chamber 无菌容器，灭菌室sterile solution 无菌溶液sterile working 无菌操作steriliser 消毒器，灭菌器sterility detector 灭菌检验器sterilization 灭菌，消毒sterilize 灭菌，消毒sterilized dressing 无菌敷料sterilizer 消毒器，灭菌器sterilizing forceps 消毒钳sterilizing lamp 灭菌灯sterilizing room 无菌室sterilometer 消毒测定器sternal 胸骨的sternal biopsy 胸骨髓活组织检查sternal knife 胸骨刀sternal needle holder 胸骨持针器sternal punch 胸骨钻孔器sternal puncture needle 胸骨穿刺针sternal retractor 胸骨牵开器sterno- 胸骨sternogoiometer 胸骨角度测量器sternotomy air saw 风动胸骨锯sternum 胸骨sternum chisel 胸骨凿sternum knife 胸骨刀sternum shears 胸骨剪stethendoscope 胸部x射线透视机stetho- 胸stethocyrtograph 胸廓曲度描记器stethogoniometer 胸廓曲度计stethograph 胸动描记器stethography ①胸动描记法②心音描记法stethokyrtograph 胸廓曲度描记器stethometer 胸围计，胸廓张度计stethophone ①胸音传播器②听诊器stethophonometer ①胸音计②听诊测音器stethopolyscope 多管听诊器（教学用）stethoscope 听诊器stethoscope chestpiece 胸部听诊头stethoscope diaphragm 听诊器薄膜stethoscope transducer 听诊器传感器stethoscopy 听诊器检查stew ①噪声②热浴室stheno- 力量sthenometer 肌力计sthenometry 体力测量法stibium (abbr. sb) 锑stick 棍，棒，操纵杆stiffness 硬度，稳定性stigma ①气孔，小孔②斑，点stigmatic ①像散校正的②小孔的stigmatometer 视网膜检视镜stigmatoscope 细孔屈光镜stilb 熙提（表面亮度单位）stilet ①通管丝，管心针②细探子③锥刺stilette ①通管丝，管心针②细探子③锥刺still 蒸馏器stilligout 点滴管stilling 蒸馏stilus ①通管丝，管心针②细探子③棒剂stimulant 兴奋剂，刺激物stimulating electrode 刺激电极stimulation 兴奋，刺激stimulation level 刺激级stimulator ①刺激器②刺激物stimulator ophthalmoscope 刺激检眼镜stimulus threshold 刺激阀stipulation ①规定，限制②合同，契约stir 搅拌stirrer ①搅拌器②搅棒stirrer bar 搅棒stirring machine 搅拌机stirring rod 搅棒stirrup 镫形件，u形卡stitch 缝线stiching instrument 缝合器stitch scissors 缝合剪stochastic 随机的，机遇的stock ①原料，存货②台，座，架stock-cutter 切料机stocking 长袜，袜套stoechiometer 化学计算器，化学计量器stoichiometer 化学计算器，化学计量器stomach 胃stomach brush 胃刷stomach catheter 胃导管stomach cells adopter 胃细胞取样器stomach clamp 胃夹，胃钳stomach evacuator 洗胃排液器stomach forceps 胃钳stomach irrigator 洗胃器stomach model 胃模型stomach pump 胃抽器，胃唧筒stomach resection and suturing clamp 胃切除缝合器stomach siphon 胃虹吸管stomach tube 胃管stomach washer 胃脏冲洗器stomat- 口，口腔stomatic 口的stomatology 口腔学stomatoscope 口腔镜stomatoscopy 口腔镜检查-stomy 造口术，吻合术stone 石，结石stone breaker 碎石器stone dislodger 取结石器stone searcher 膀胱石探杆（检查膀胱石用）stools ①凳子②托架，座stop ①停止②制动器③光圈stopcock 开关，活塞，龙头stop-needle 有档针stopper ①充填器②塞子③制动器stop speculum 固定开睑器stop watch 秒表，跑表storage ①储藏，储存②仓库，存储器storage battery 蓄电池组storage cabinet 储藏柜storage capsule 储存容器storage cell 蓄电池storage oscilloscope 存储示波器store 记忆装置，存储器story 故事，经历stove 炉子，加热器stoving machine 烘干机s.t.p. (standard temperature and pressure) 标准温度和压力str (systolic time intervals) 收缩时间间期（心脏）strabism 斜视，斜眼strabismometer 斜视计strabismus forceps 斜视镊strabismus hook 斜视钩strabismus knife 斜视刀strabismus needle 斜视眼针strabismus scissors 斜视剪strabometer 斜视计strabotome 斜视刀straight 直的，直线straight adapter 直接管straight angle 平角straight b/l 直运提单straight handpiece 直机头straight knife 直刀strain ①张力，应变②过滤strainer 滤过器strain gauge 拉力计，应变计strain tube 应变管strand 线，导线束，丝条strap 皮带，条带stratification 层，层次stratigram x射线断层图，x射线体层照片stratigraphy 体层x射线照像术，断层x射线照像术stratum 层streak 条纹，划线stream 流，气流，水流street (abbr.st.;str.) 街道s trength ①体力，力量②强度③浓度strephotome 螺钻形刀stress 压力，张力，应力stress amplifier 应变压力放大器stress brdaker 应力中断器stretch 伸展，拉长stretcher ①担架②拉直器stretching pliers 扩张钳striascope 屈光检查器striation 纹，条纹strict 严格的，精确的stricture 狭窄stricture explorer 检狭窄探杆stricturoscope 直肠狭窄镜stricturotome 直肠狭窄切开刀string electrometer 弦线电流计string galvanometer 弦线电流计strip ①磨带，条②剥离strip-cutter 切条器strip penetrameter 条状x射线透度计stripper 剥离器strobe ①闸门②闪频观测器strobolaryngoscope 动态喉镜，回旋喉镜stroboscope ①动态镜②闪光仪stroboscopic disc 动态镜盘，斜视镜盘strobostereoscope 立体动态镜stroke 发作，冲程stroke volume (abbr. sv) 心搏排血量stromuhr 血流速度计strong 强的，有力的strong anion exchanger 强阴离子交换器（色谱法）strong cation exchanger 强阳离子交换器strontium (abbr. sr) 锶strontium ophthalmic applicator 眼科用sr90敷贴器structure 结构，构成struggle 斗争s-t segment s-t节段（心电图）stud 大头钉，栓钉student microscope 教学显微镜study model 研究模型stuff 材料，原料stump bur 牙残根钻stump elevator 牙残根梃子stump file 牙残根锉stump splinter forceps 牙残根碎片钳style ①式样，型②描笔③细探子，管心针stylet ①通管心针，通管丝②细探子stylet mandrel 管心针stylus ①描笔，记录笔②细探子，通管丝，管心针stylus tracer 细探子描记器（牙科）stype 药栓，药布styptic cotton 止血棉sthptic sponge 止血海绵sub- 在下面，亚，不足，副subarachnoid screw 蛛网膜下螺丝subarachnoid screw driver 蛛网膜下螺丝装拆器subarachnoid twist drill 蛛网膜下旋钻subassembly ①组件，机组②局部装配subaudible 次声（频）的subcutaneous 皮下的subinfuse-port 皮下埋藏灌注器subcutaneous syringe 皮下注射器subdermal 皮下的subaermal needle electrod 皮下针状电极（eeg）subdivision ①细分，重分②一部分subduce 扣除，减去subintegumental electrode 皮下电极subject ①主题，学科②使从属subjective 主观的，自觉的subjective photometer 直观光度计subjective refraction system 自动验光系统subjectoscope 视觉检查器subject range 适应范围sublimating apparatus 升华器sublimation 升华（作用）sublimator 升华器subliminal 阈下的，限下的sublingual 舌下的sublingual tablet 舌下片submicroscopic 亚显微的，亚微观的subminiaturization 超小型化subnormal 低常的，正常以下的subordinate ①部属的，次的②辅助的subprogram 子程序subscriber ①订户，用户②签名人subscript 记号，标记，脚注subsequence ①顺序，序列②后，次subsequent 以后的，次的subsidiary 辅助的，副的subsonic vibration 次声振动substage 镜台下部（显微镜）substage lamp 镜台下灯（显微镜）substance ①物质，材料②内容substandard 副标准，标准下的substitution 代替，取代，置换substrate ①基片，补底②底物subsystem 辅助系统subterminal 终端下的subthalmogram 丘脑底部图subthreshold stimulus 阈下刺激物subthreshold summation 阈下总和subtraction 减去法（放射诊断学）subtraction unit （x射线）减法装置subtractive 减去的，负的subtractor 减法器，减数subzero 零下，负的succedaneum 代用品，替代品succeed ①成功，及格②接替success 成功，成就succession 连续，系列suck 吮，吸suck and blow apparatus 吸吹式人工呼吸器sucked type 吸盘式sucker 吸盘，吸管，吸入器sucker apparatus 吸器，吸盘sucker tube 吸盘管suction ①吸，抽吸②抽吸器suction apparatus 吸引器suction booster 吸引增压器suction bottle 吸引瓶，吸滤瓶suction chamber 吸室suction cup 吸杯suction curet 吸引刮匙suction filter 吸滤器suction flask 吸滤瓶suction nozzle 吸气管suction-pipe 吸管，抽气管suction pump 抽气泵，吸气唧筒suction tube 吸引管，吸管suction unit 吸引器sufficiency 充足，足量sugar 糖sugarcoating machine 包糖衣机suggestion 建议，提出，意见suit ①适合，适应②套，组sulf- 硫，磺基sulfate 硫酸盐sulfur (abbr. s) 硫sulfurator 硫磺熏蒸器sulfuric acid 硫酸sulphuric acid desiccator 硫酸干燥器sum 总数，合计summary 摘要，大略summation 合计，总和summit 顶点，最高峰sump 池，坑，贮槽sump suction tube 池吸管sun-bath 日光浴sunday (abbr.sun.) 星期日sunlight 太阳光sunlight lamp 日光灯sun-parlor 日光浴室super 特级的，优等的super- 在…上，过度super-audio 超音频supercentrifuge 超速离心机supercharge 增压supercharger 增压器superconductor 超导体supercooled 过冷的superficial 表面的，肤浅的superficial scaler 表层刮器（用以去除齿龈结石）superficial therapy x-ray equipment x射线浅部治疗机superficial x-ray treatment x射线浅层治疗superheterodyne spectrometer 超外差分光计superiority 优秀，优越性superior limit 上限super low frequency therapeutic apparatus 超低频治疗机supernatant ①漂浮的②上层清液superperformance 超级性能，良好性能super-pressure kettle 高压锅superscope 超宽银幕电影superscriiption 处方标记，取supersonic 超声波的，超音频的supersonic detector 超声波检测器supersonic diagnostic set 超声波诊断仪supersonic echo sounder 超声波回声探测仪supersonic frequency 超声频率supersonic generator 超声波发生器supersonics 超声波，超声波学supersonic sounding 超声探测supersonic vibration 超声振动supersonic wave 超声波supertension 超高压supervision 监视，管理supervoltage 超电压，超高压supervoltage generator 超高压发电机super widefield condenser 超宽视野聚光器super widefield eyepiece 超宽视野接目镜supplement 补充，增刊，附录supplier 供给者supply ①供给，输送②电源supply cabinet 供应柜supply main 供电干线supply room 供应室supply voltage 供给电压support ①支柱，支架②底座supposition 假定，推测suppository 栓剂suppository desintegrationtester 栓剂溶介测定仪suppository machine 栓药机suppository mould 栓剂模型suppress 抑制，压制suppressor 抑制器，消除器supra- 上，在……之上supraliminal stimulus 阈上刺激物suprapubic catheter 耻骨上导尿管suprapubic urinal 耻骨上贮尿器suprarene 肾上腺surface 面，表面surface absorber 表面吸收器surface adsorption 表面吸附surface applicator 表面贴敷器surface biopsy 表面活组织检查surface electrode 表面电极surface stimulating electrode 表面刺激电极surface tension 表面张力surface tensometer 表面张力测定器surface thermometer 表面温度计surfactant 表面活性剂surgeon's needle 外科针surgeon's needle holder 持针器surgery 外科surgery microscope 手术显微镜surge suppressor 突波遏抑器surgical bed 手术床surgical blade 手术刀片surgical bur 外科钻surgical cement 外科粘固粉surgical diathermy unit 电手术器surgical olrape 外科手术巾surgical drill 手术钻surgical electrode 外用电极surgical forceps 手术镊surgical knot 外科结surgical mallet 外科锤surgical mask 手术口罩surgical mesh 心脏修补网状织物surgical monitor 手术监护仪surgical pad 手术橡皮垫surgical paraffin 外科用石腊surgical pliers 手术镊surgical scissors 手术剪surgical spoon 手术匙surgical suture needle 外科缝合针surgical tray 手术盘surgical unit 手术仪器surmount 克服，打破survey ①观察，调查②测量survey line 观测线surveyor ①测量器②测量员survey report 检验报告susceptance 电纳susceptibility ①灵敏度②磁化率susceptible 灵敏的，敏感的susceptiveness 灵敏性，敏感性susceptor 感受器suscitation 兴奋，刺激suspect 怀疑，推测suspend 推迟，暂停，悬挂suspended magnet 悬式吸铁器suspender 悬吊带，悬吊器suspensiometer 混悬度测定器suspension ①悬吊②悬吊架③悬浮液suspension splint 悬吊夹suspensory bandage 悬吊绷带sustain 支持，经受sutures 手术缝线，缝术suture bobbin 缝合线轴suture clip 缝合夹suture clip applying and removing forceps 创缘夹缝拆镊suture clip applying forceps 创缘夹缝合镊suture cutting forceps 缝合切割钳suture forceps 缝线钳suture guide 缝线导子suture instruments 缝合器械suture needle 缝合针suture pliers 缝针镊suture ring 缝合环suture scissors 缝合剪suture silk 缝合线suture tag forceps 缝合结节钳suture tying forceps 打线结钳suture wire scissors 缝线剪sv (stroke volume) 心搏出量svcg (spatial vectorcardiogram) 空间心电向量图svec (stereovectorelectrooardiogram) 立体心电向量图s. w. (specific weight) 比重swab 拭子swab stick 拭子条swage 铁模swager 牙压模器swan socket 插入式插座，卡口灯座swap 交换，交叉swedged needle 带缝线针sweep ①扫描②长，宽，高度sweep check 扫频检验sweep electron microscope 扫描式电子显微镜sweep reflectometer 扫频反射计swift 快，迅速swim ①游，游泳②漂浮swing ①摆动，回转②悬腿架swing bed 摇床swinging ball mill 振荡式球磨机swing-out 摆动式swing-out filter holder 摆动式持滤光镜架swing-out stirrer 摆动式搅拌器swing-type centrifuge 摇摆式离心机switch 闸，开关，电键switchboard 配电盘，电键板switcher 转换开关switch-fuse 开关保险丝switch in 接入，合闸switching ①配电，转换②开关switching amplifier 转换放大器switching box 转换盒switch off 切断，关掉switch on 开，接通switch panel 开关板switch selectro 选键器switch unit 转换开关swivel 旋转，转体swivel head examining lamp 转头检查灯swivel knife 旋转刀swivel stirrup 旋回牵引镫sylvatron 电光管sym- 连，合，共symballophone 定向听诊器symbol 符号，象征symbolize 用符号表示symmetric(al) 对称的，匀称的symmetrization 对称化symmetry 对称，匀称sympathectomy dissector 交感神经剥离器sympathectomy hook 交感神经钩symphysiotome 耻骨联合刀symphysiotomy knife 耻骨联合切开刀symposium 经验交流，讨论会symptom 症状symptomatography 症状记录synapse ①突触，神经键②联合synaptic potential 突触电位sync ①同步②同步机sync defibrillator 同步除颤器syncelom 体腔synchro- ①同步②同步机synchro-cyclotron 同步电子回旋加速器synchrometer 同步计synchronism 同步性，同时性synchronization 同步，同期synchronized pulmotor 同步呼吸机synchronizer 同步机，同步装置synchronous 同步的synchronous pacemaker 同步起搏器synchronous timer 同步定时器synchroscope 同步示波器synchrotone 同步超声发生器synchrotron 同步加速器syndrome 综合征synechia knife 虹膜粘连切开刀synechotome 虹膜粘连切开刀synopsis ①概要，内容摘要②对照表，说明书synoptophore 同视机，斜视诊疗器synoptoscope 同视镜，斜视检眼镜synteresis 预防synthermal 等温的synthescope 合成观测器synthesis 合成，综合synthesizer 合成器，综合器synthetic 合成的，人造的synthetic eye 人造眼，假眼synthetic membrane 人工膜syntony 谐振，共振syphon 虹吸管syringe 注射器，灌注器syringe adapter 注射器接头syringe burette 注射滴定管syringe hydrometer 吸管式比重计syringe needle 注射器针头syringe nozzle 注射器头syringe pipe 冲洗管，冲洗头syringo- 瘘管syringotome 瘘管刀system 系统，装置，设备systematic 有系统的，有规则的systematization 系统化，分类system compstibility guarantee 系统兼容性的保证书systemic circulation 体循环system simulation 系统模拟systole 收缩期（心脏）systolic 收缩的systolometer 心音鉴定器。
Metal Abundances of one Hundred Hipparcos Dwarfs
a r X i v :a s t r o -p h /9707060v 1 4 J u l 1997METAL ABUNDANCES OF ONE HUNDRED HIPPARCOS DW ARFSR.G.Gratton 1,E.Carretta 2,G.Clementini 2,C.Sneden 31Osservatorio Astronomico di Padova,Vicolo dell’Osservatorio 5,35122Padova,ITALY2Osservatorio Astronomico di Bologna,ITALY3Department of Astronomy,The University of Texas at AustinABSTRACTAbundances for Fe,O,and the α−elements (Mg,Si,Ca,and Ti)have been derived from high resolution spectra of a sample of about one hundred dwarfs with high precision parallaxes measured by HIPPAR-COS.The stars have metal abundances in the range −2.5<[Fe/H]<0.2.The observational data set con-sists of high dispersion (20,000<R <70,000),high S/N (>200)spectra collected at the Asiago and McDonald Observatories.The abundance analysis followed the same precepts used by Gratton et al.(1997a)for ∼300field stars and for giants in 24glob-ular clusters (Carretta &Gratton 1997),and includes corrections for departures from LTE in the formation of O lines.Our main results are:1.the equilibrium of ionization of Fe is well satisfied in late F –early K dwarfs2.O and α−elements are overabundant by ∼0.3dex This large homogeneous data set was used in the derivation of accurate ages for globular clusters (See paper by Gratton et al.at this same Meeting).Key words:Stars:chemical abundances -Stars:ba-sic parameters1.INTRODUCTIONHIPPARCOS has provided parallaxes with accura-cies of ∼1mas for several hundreds dwarfs.We had access to data for about 100dwarfs with metal abun-dances in the range −2.5<[Fe/H]<0.2and have used them in a thorough revision of the ages of the old-est globular clusters derived by Main Sequence (MS)fitting technique.A crucial step in the derivation of ages via this method is the assumption that the nearby subdwarfs have the same chemical composi-tion of the globular cluster main sequence stars.This assumption was verified through a careful abundance analysis of the vast majority of nearby dwarfs with HIPPARCOS parallaxes available to us.Our data set and the HIPPARCOS parallaxes were also used to test whether an appreciable Fe overion-ization occurred in the atmosphere of late F –early K dwarfs (Bikmaev et al.1990;Magain &Zhao 1996).This was done by comparing abundances provided by neutral and singly ionized lines,once the surface gravity of each program star had be derived from its mass,temperature and luminosity rather then from the equilibrium of ionization of Fe.Finally,our abundances are fully consistent with those presented by Gratton et al.(1997a)for about 300field dwarfs.A large,homogenous data base of high accuracy (errors ∼0.07dex)abundances com-puted with the Kurucz (1993)model atmospheres is now available and can be used to recalibrate photo-metric and low S/N spectroscopic abundances.2.BASIC DATA FOR SUBDWARFS Average V magnitudes and colors (Johnson B −V and V −K ,and Str¨o mgren b −y ,m 1and c 1)for the programme stars were obtained from a careful discussion of the literature data.We used also the Tycho V magnitudes and B −V colors,after cor-recting them for the very small systematic difference with ground-based data.Absolute magnitudes M V were derived combining ap-parent V magnitudes and Hipparcos parallaxes.No Lutz-Kelker corrections were applied.Lutz-Kelker corrections (Lutz &Kelker 1973)take into account that stars with parallaxes measured too high are more likely to be included in a sample if the sample selection criteria are based on the parallaxes them-selves.Since our sample was selected before the HIP-PARCOS parallaxes were known;Lutz-Kelker correc-tions should not be applied when the whole sample is considered,as we do when comparing the abundances obtained from Fe I and Fe II lines.Multiple high precision radial velocity observations exist for a large fraction of our objects (80out of 99).Twenty stars in the sample are known and four are suspected spectroscopic binaries.Two further stars display very broad lines in our spectra,possibly due to fast rotation.They were discarded.A few other stars display some IR excess,which also may be a signature of binarity.No evidence for binarity dis-turbing the present analysis exists for the remaining stars.Sixty-eight out of the99stars of our sample are in-cluded in Carney et al.(1994)catalogue.Reddening estimates are given for58of them.All but two have zero values.We have thus assumed a zero reddening for all the programme stars.3.OBSERVATIONS AND REDUCTIONSHigh dispersion spectra for about two thirds of the programme stars were acquired using the2D-coud`e spectrograph of the2.7m telescope at McDonald Ob-servatory and the REOSC echelle spectrograph at the 1.8m telescope at Cima Ekar(Asiago).McDonald spectra have a resolution R=70,000,S/N∼200, and spectral coverage from about4,000to9,000˚A; they are available for21stars(most with[Fe/H]<−0.8).Cima Ekar telescope provided spectra with resolution R=15,000,S/N∼200,and two spectral ranges(4,500<λ<7,000and5,500<λ<8,000˚A) for65stars.Equivalent widths EW s of the lines were measured by means of a gaussianfitting routine applied to the core of the lines;appropriate average corrections were included to take into account the contribution of the damping wings.Only lines with log EW/λ<−4.7 were used in thefinal analysis(corrections to the EW s for these lines are≤7m˚A,that is well be-low10per cent).The large overlap between the two samples(14stars)allowed us to tie the Asiago EW s to the McDonald ones.External checks on our EW s are possible with Ed-vardsson et al(1993:hereinafter E93)and Tomkin et al.(1992:hereinafter TLLS).Comparisons per-formed using McDonald EW s alone show that they have errors of±4m˚A.From the r.m.s.scatter,σ, between Asiago and McDonald EW s,we estimate that the former have errors of±6.7m˚A.When Asi-ago and McDonald EW s are considered together,we find average residuals(us-others)of−0.2±1.0m˚A (39lines,σ=6.1m˚A)and+0.8±1.0m˚A(36lines,σ=5.9m˚A)with E93and TLLS,respectively.4.ANALYSIS4.1.Atmospheric ParametersThe abundance derivation followed precepts very similar to the reanalysis of∼300field and∼150 globular cluster stars described in Gratton et al. (1997a)and Carretta&Gratton(1997).The same line parameters were adopted.The effective tem-peratures were derived from B−V,b−y,and V−K colours using the iterative procedure outlined in Gratton et al.(1997a).Atmospheric parameters are derived as follows:1.we assume as input values log g=4.5and themetal abundance derived from the uvby photom-etry using the calibration of Schuster&Nissen (1989)2.T effis then derived from the colours,using theempirical calibration of Gratton et al.(1997a) for population I stars(assumed to be valid for [Fe/H]=0),and the abundance dependence given by Kurucz(1993)models3.afirst iteration value of log g is then derived fromthe absolute bolometric magnitude(derived from the apparent V magnitude,parallaxes from Hip-parcos,and bolometric corrections BC from Ku-rucz1993),and masses obtained by interpolation in T effand[A/H]within the Bertelli et al.(1997) isochrones4.steps2and3are iterated until a consistent setof values is obtained for T eff,log g,and[A/H] 5.the EW s are then analyzed,providing new val-ues for v t and[A/H](assumed to be equal to [Fe/H]obtained from neutral lines)6.the procedure is iterated until a new consistentset of parameters is obtained4.2.Error analysisRandom errors in T eff(±45K)were obtained by com-paring temperatures derived from different colours. Systematic errors may be larger;the T eff-scale used in this paper is discussed in detail in Gratton et al. (1997a).We assume that systematic errors in the adopted T eff’s are≤100K.Random errors in the gravities(±0.09dex)are esti-mated from the errors in the masses(1.2per cent), M V’s(0.18mag),and in the T eff’s(0.8per cent), neglecting the small contribution due to BC’s.Sys-tematic errors(±0.04dex)are mainly due to errors in the T effscale and in the solar M V value.Random errors in the microturbulent velocities can be estimated from the residuals around thefitting re-lation in T effand log g.We obtain values of0.47and 0.17km s−1for the Asiago and McDonald spectra, respectively.Random errors in the EW s and the line parameters significantly affect the abundances when few lines are measured for a given specie.Errors should scale as σ/√Figure1.Run of the difference between the abundances derived from neutral and singly ionized Fe lines as a func-tion of temperature(panel a)and overall metal abundance (panel b).Open squares are abundances obtained from the Asiago spectra;filled squares are abundances obtained from the McDonald spectraMcDonald spectra,respectively.Systematic errors (∼0.08dex)are mainly due to the T effscale.parison with other abundancesOn average,differences(Asiago−McDonald)in the Fe abundances are−0.01±0.02dex(12stars,σ= 0.07dex).Analogous differences for the[O/Fe] and[α/Fe]ratios are+0.02±0.08dex(5stars,σ=0.17dex),and+0.01±0.03dex(12stars,σ=0.10dex).E93measured abundances for∼200dwarfs;six stars are in common with our sample.Abundance residu-als(our analysis−E93)are+0.08±0.03,−0.02±0.03, and+0.02±0.02dex for[Fe/H],[O/Fe],and[α/Fe], respectively.Residual differences are mainly due to our use of a higher temperature scale(our T eff’s are larger by63±12K).We have six stars in common with TLLS,which used a restricted wave-length range.Average differences(ours−TLLS)are: +0.34±0.04and−0.31±0.07dex for[Fe/H]and [O/Fe],respectively.They are due to different as-sumption in the analysis:(i)our temperature scale is higher;(ii)TLLS used a different solar model; (iii)our non-LTE corrections to the O abundances are slightly larger.Finally,Gratton et al.(1997a) made a homogenous reanalysis of the original EW s for∼300metal-poorfield stars.On average,the present Fe abundances are larger by0.02±0.02dex (11stars,σ=0.06dex).Since the same analysis procedure is adopted,these differences are entirely due to random errors in the EW s and in the adopted colours.In the following,we assume that Gratton et al.abundances are on the same scale of the present analysis.4.4.Fe abundancesSince gravities are derived from masses and luminosi-ties rather than from the equilibrium of ionization for Fe,we may test if predictions based on LTE are sat-isfied for the program stars.In Figure1we plot the difference between abun-dances of Fe obtained from neutral and singly ion-ized lines against effective temperature and metal abundance.Different symbols refer to results ob-tained from McDonald and Asiago spectra,respec-tively.McDonald spectra have a higher weight be-cause the higher resolution allowed us to measure a larger number of Fe II lines(10∼20),and errors in the EW s are smaller;very few Fe II lines could be measured in the crowded spectra of cool and/or metal-rich stars observed from Asiago.Average dif-ferences between abundances given by Fe I and II lines are0.025±0.020(21stars,σ=0.093dex)for the Mc Donald spectra,and−0.063±0.019(52stars,σ=0.140dex)for the Asiago spectra.The scatter obtained for McDonald spectra agrees quite well with the expected random error of0.085dex.The average value is consistent with LTE if the adopted T effscale is too high by∼20K,well within the quoted error bar of±100K.The lower mean difference obtained for the Asiago spectra is due to a few cool metal-rich stars which have very crowded spectra.Very few Fe II lines could be measured in these spectra and the line-to-line comparison with the superior McDonald data suggests that even these lines may be affected by blends.We conclude that the equilibrium of ionization for Fe is well satisfied in the late F–K dwarfs of any metallicity in our sample.This result depends on the adopted temperature scale.Our empirical result agrees very well with the ex-tensive statistical equilibrium calculations for Fe by Gratton et al.(1997b).In that paper,the uncertain collisional cross sections were normalized in order to reproduce the observations of the RR Lyraes,where overionization is expected to be much larger than in late F–K dwarfs.The lower limit to collisional cross sections given by the absence of detectable overion-ization in RR Lyrae spectra(Clementini et al.1995) implies that LTE is a very good approximation for the formation of Fe lines in dwarfs.4.5.O andα−element abundancesO abundances were derived from the permitted IR triplet,and include non-LTE corrections computed for each line in each star following the precepts of Gratton et al.(1997b).Wefind that O and the other α−elements are overabundant in stars with[Fe/H]<−0.5(see Figure2):[O/Fe]=0.38±0.13[α/Fe]=0.26±0.08,(error bars are the r.m.s.scatter of individual val-ues around the mean).The moderate O excess de-rived from the IR permitted lines is a consequence of the rather high temperature scale adopted.When this adoption is made,abundances from permitted OI lines agree with those determined from the forbidden [OI]and the OH lines.The present abundances agree very well with those derived in Gratton et al.(1997c).Note also that the overabundance of O andα−elements found for thefield subdwarfs is similar to the excesses foundFigure2.Runs of the overabundances of O(panel a)and α−elements(panel b)as a function of[Fe/H]for the pro-gramme subdwarfs.Filled squares are abundances from McDonald spectra;open squares are abundances from Asi-ago spectrafor globular cluster giants(apart from those stars af-fected by the O-Na anticorrelation,see Kraft1994).5.CALIBRATION OF PHOTOMETRICABUNDANCESOnce combined with the abundances obtained by Gratton et al.(1997a),the sample of late F to early K-typefield stars with homogenous and accu-rate high dispersion abundances adds up to nearly 400stars.Schuster&Nissen(1989)have shown that rather accurate metal abundances for late F to early K-type can be obtained using Str¨o mgren uvby pho-tometry(available for a considerable fraction of the HIPPARCOS stars).Furthermore,the extensive bi-nary search by Carney et al.(1994)has provided a large number of metal abundances derived from an empirical calibration of the cross correlation dips for metal-poor dwarfs.We have recalibrated these abundance scales.Schus-ter&Nissen(1989)abundances onlydiffers for a zero-point offset(see panel a of Figure3);the mean difference is:[Fe/H]us =[Fe/H]SN+(0.102±0.012),(1)based on152stars(the r.m.s.scatter for a single star is0.151dex).In the case of Carney et al.(1994,panel b of Fig-ure3),a small linear term is also required.The best parison between the abundances obtained from high dispersion spectra(present analysis or Gratton et al.1997),and those provided by the original calibration of Schuster&Nissen(1989,panel a)and Carney et al. (1994,panel b)fit line(66stars)is:[Fe/H]us=(0.94±0.03)[Fe/H]C94+(0.18±0.17),(2) The offsets between the high dispersion abundances and those provided by Schuster&Nissen(1989)and Carney et al.(1994)are mainly due to different as-sumptions about the solar abundances in the high dispersion analyses originally used in the calibrations of Schuster&Nissen(1989)and Carney et al.(1994).REFERENCESBertelli,P.,Girardi,L.,Bressan,A.,Chiosi,C.,&Nasi,E.1997,in preparationBikmaev,I.F.,Bobritskij,S.S.,El’kin,V.G.,Lyashko,D.A.,Mashonkina,L.I.,&Sakhibullin,N.A.1990,inIAU Symp.145,Evolution of Stars:the Photospheric Abundance Connection,G.Michaud ed.Carney,B.W.,Latham,D.W.,Laird,J.B.,&Aguilar, L.A.1994,AJ,107,2240Carretta,E.,&Gratton,R.G.1997,A&AS,121,95 Clementini,G.,Carretta,E.,Gratton,R.G.,Merighi, R.,Mould,J.R.,&McCarthy,J.K.1995,AJ,110, 2319Edvardsson,B.,Andersen,J.,Gustafsson,B.,Lambert,D.L.,Nissen,P.E.,&Tomkin,J.1993,A&A,275,101Gratton,R.G.,Carretta,E.,&Castelli,F.1997a,A&A, in pressGratton,R.G.,Carretta,E.,Gustafsson,B.,&Eriksson, K.1997b,submitted to A&AGratton,R.G.,Carretta,E.,Matteucci,F.,&Sneden,C.1997d in preparationKing,J.R.1993,AJ,106,1206Kraft,R.P.1994,PASP,106,553Kurucz,R.L.1993,CD-ROM13and CD-ROM18 Lutz,T.E.,Kelker,D.H.1973,PASP,85,573 Magain,P.,Zhao,G.1996,A&A,305,245Schuster,W.J.,&Nissen,P.E.1989,A&A,221,65 Tomkin,J.,Lemke,M.,Lambert,D.L.,&Sneden,C.1992,AJ,104,1568。
Landsat Explorer App使用指南说明书
Over the past 43 years, Landsat has amassed over four million scenes of data, taking images of every location on earth every 16 days. Using the Landsat app, you can explore historic images to see how places change over time and look at images using different combinations of spectral bands. In this exercise, you will investigate three features of the Landsat Explorer app.You have been asked to demonstrate the Landsat Explorer app to a group of learners without previous experience using Landsat. You need to analyze four different locations. You must qualitatively and quantitatively examine the locationBuild skills in these areasOpening the Landsat appFinding locations using addressesUsing different spectral band combinationsAnalyzing various spectral profilesAccessing metadata about the imageryWhat you needAccount not requiredEstimated time: 30 minutes to 1 hourPublication date: March 14, 20191. Features of the Landsat Explorer app1. The app provides quick access to the following band combinations:•Agriculture: Highlights agriculture in bright green. Bands 6,5,2•Natural Color: Sharpened with 25m panchromatic band. Bands 4,3,2+8•Color Infrared: Healthy vegetation is bright red. Bands 5,4,3•SWIR (Short Wave Infrared): Highlights rock formations. Bands 7,6,4•Geology: Highlights geologic features. Bands 7,4,2•Bathymetric: Highlights underwater features. Bands 4,3,1•Panchromatic: Panchromatic image at 15m. Band 8•Vegetation Index: Normalized Difference Vegetation Index (NDVI).(Band5-Band4)/(Band5+Band4)•Moisture Index: Normalized Difference Moisture Index (NDMI). (Band5-Band6)/(Band5+Band6)2. The Time tool enables access to a time slider and temporal profile fordifferent indices based on a selected point. The Time tool is onlyaccessible at large zoom scales. It also provides temporal profiles forNormalized Difference Vegetation Index (NDVI), Normalized DifferenceMoisture Index (NDMI), and an Urban Index.3. The Identify tool enables access to information on the scenes and canalso provide a spectral profile based on a selected point.2. Washington, DC – urban area1. Open the Landsat Explorer app.2. Search for Washington, DC, District of Columbia, United States.The Landsat view opens in Natural Color. In this view, you can clearly see the bridges, highways and concentrated developed land.3. Change the Band combination to color infrared, which shows healthy vegetationas bright red. Click the third icon down on the left panel.4. Locate Arlington Cemetery and the golf course to the West of Addison Heights. IfAddison Heights is not immediately visible, zoom in another level.Spectral profiles indicate the value of each pixel for each band. They areessentially plots of the reflected radiation of different objects. Objects behave differently with different wavelengths and therefore they have different spectral profiles. In this next section, you will examine the spectral profile of water,developed land, and healthy vegetation.5. Click i (for information) and click on water in the image.You get information about the Landsat scene as well as a spectral profile.Typical spectral profiles are shown as well as the profile of the pixel youselected. Notice that the values are relatively low throughout all the bands.This is because water absorbs light and does not reflect as much as otherobjects.6. Click i and get a spectral profile of developed land.Q1. Describe the spectral profile curve for development land, paying attention to where the profile spikes.7. Click i and get a spectral profile of healthy vegetation.Q2. Describe the spectral profile curve for healthy vegetation. Why does it spike to the NIR band?8. Check all the Typical Spectral Profiles.Q3 Looking at all the Spectral Profiles, write a summary of how spectralreflectance is reflected in the spectral profiles of different objects.3. Wadi As-Suh, Saudi Arabia—agriculturalAreaCircular irrigation is a method of crop irrigation in which equipment rotatesaround and waters crops with sprinklers. In this section of the exercise, you willidentify areas of circular irrigation and examine them using both the vegetationand moisture indexes.1. Search for Wadi As-Sirhan, Saudi Arabia2. Show the image using the Vegetation Index that shows healthy vegetation indark green.3. Show the image using the Moisture Index where moisture-rich areas are brightblue.Q4 Which band combination shows the circular fields the best?4. Princess Charlotte Bay, Queensland,Australia—ocean areaCoral reefs, under threat from environmental conditions, can be monitored byremote satellite imagery. Using remote sensing data, coral reefs can be classified by structure and type and these classifications can be compared temporarily toshow change. Find and identify the coral reefs in the area identified.1. Search for Princess Charlotte Bay, Queensland, Australia.2. Display the image using the Bathymetric band combination.Q5 What color displays the coral reefs?Q6 Calculate a spectral profile for the ocean.Q7 Calculate a spectral profile for the coral reef.Q8 How do the two spectral profiles compare?5. Abu Dhabi – desert areaEolian formations are found in places where wind is the cause of erosion anddeposition.Eolian sediments are usually materials that consist of sand and silt-sizedparticles. Remote sensing can provide valuable information about regionalgeomorphologic features caused by wind. The study of eolian formations helpsus understand climate and the forces mold it.1. Search for Abu Dhabi, United Arab Emirates and zoom until you see an imagethat matches the image shown here.2. Display using the geology band combination.3. Zoom out and look for the eolian formations.4. Describe one pattern of an eolian formation.5. To observe the dunes and orientation better, display as Panchromatic for asharper image in black and white.Copyright © 2018 Esri. All rights reserved.https:///。
载波相位观测值英语
载波相位观测值英语When it comes to GPS positioning, carrier phase observations are like the fine-tuned instrument readings. They're those precise measurements that help us determine the exact position of a receiver down to a fraction of a wavelength.In the world of satellite navigation, carrier phase observations are kind of like the secret sauce. You don't often hear about them, but they're what makes the magic happen. It's like when you're cooking and add that special ingredient that takes the dish to the next level.Think of carrier phase observations as the high-resolution photos of the sky. They capture the tiny details that other methods miss, giving us an incredibly accurate picture of where we are. It's like zooming in on asatellite image and seeing things you never noticed before.Carrier phase observations are like the dance betweensatellites and receivers. They're these delicate measurements that require precision timing and synchronization. It's like a ballet, with each satellite and receiver playing their part perfectly to create a harmonious whole.In the jargon of GPS enthusiasts, carrier phase observations are the holy grail. They're the gold standard, the benchmark that all other positioning methods aspire to match. It's like having the perfect score in a game everyone knows you've achieved something special.。
6.Isolators
two polarizers. In practice the FR is a saturated Bi:RIG iron garnet (cf. §4.2.3)
where the magnetization is fixed by a permanent magnet, such as Sm-Co, or
In the forward, or transmission, direction, the lead polarizer Po polarizes the light along the horizontal (the absolute direction being, of course, imma-
where the iron garnet is latching and pre-poled. Multi-magnet schemes have
been proposed to concentrate the magnetic field around the FR [5, 6, 18],
but in practice a single magnet is used. The FR is designed to rotate a linear polarization state by +45◦ (or −45◦) irrespective of transit direction.
(6.1.1)
The Faraday rotation angle θF for a plate of length L is
θF = θF L
(6.1.2)
At a nominal temperature, wavelength, and thickness the target rotation is θF o. The actual rotation for small deviations is θF = θF o + ∆θF , where the total deviation from the target is
Open and closed CDM isocurvature models contrasted with the CMB data
a r X i v :a s t r o -p h /0108422v 2 7 D e c 2001HIP-2001-48/TH astro-ph/0108422Phys.Rev.D 65,0230XXOpen and closed CDM isocurvature models contrasted with the CMB dataKari Enqvist ∗Department of Physical Sciences,University of Helsinki,and Helsinki Institute of Physics,P.O.Box 64,FIN-00014University of Helsinki,FinlandHannu Kurki-Suonio †and Jussi V¨a liviita ‡Department of Physical Sciences,University of Helsinki,P.O.Box 64,FIN-00014University of Helsinki,Finland(August 27,2001)We consider pure isocurvature cold dark matter models in the case of open and closed universes.We allow for a large spectral tilt and scan the 6-dimensional parameter space for the best fit to the COBE,Boomerang,and Maxima-1data.Taking into account constraints from large-scale structure and big bang nucleosynthesis,we find a best fit with χ2=121,which is to be compared to χ2=44of a flat adiabatic reference model.Hence the current data strongly disfavor pure isocurvature perturbations.I.INTRODUCTIONThe recent measurements of the cosmic microwave background (CMB)temperature fluctuations by the Boomerang [1,2]and Maxima-1[3,4]balloon experiments and the DASI interferometer [5]have widely been re-garded as indicating that we live in a Ω=1universe.This is so because the first acoustic peak is found at the multipole ℓ≃200,implying a flat universe.The firmness of such a conclusion is,however,based on certain tacit as-sumptions.In particular,when fitting the acoustic peak positions,one often assumes that the primordial pertur-bations are adiabatic and that the spectrum is nearly scale invariant.If perturbations are adiabatic,the relative abundances of particle species are equal to their thermal equilibrium values.This is the case in the simplest,one-field infla-tion models but it is not a generic feature of inflation.More generally,perturbations can be either adiabatic or nonadiabatic;the latter would be perturbations in the particle number densities,or entropy perturbations,and are called isocurvature perturbations.Because no generally accepted theory of inflation ex-ists,it is natural to consider both adiabatic and isocur-vature perturbations as being equally probable.This is the generic situation when more than one field is excited during inflation,such as is the case in double inflation [6]or in the minimally supersymmetric standard model with flat directions [7].One should also note that in the pre-big-bang scenario,which has been proposed as an alternative to the inflationary universe,pre-big-bang axion field fluctuations give rise to an isocurvature per-turbation spectrum [8].Purely isocurvature Ω=1per-turbations are,however,not consistent [9–11]with theobservational data,but an admixture of (uncorrelated or correlated)adiabatic and isocurvature perturbations cannot be ruled out [11–14].However,if we do not insist on a flat universe,the situation could be different.Recently,it was pointed out [15]that in the general (Gaussian)case the scalar power spectrum is a 5×5matrix P ij (k )= A i (k )A j (−k ) ,where i,j label one adi-abatic and four isocurvature modes [cold dark matter (CDM),baryon,neutrino density,and neutrino velocity]and their correlations.Here we shall focus on a purely isocurvature primordial perturbation in the CDM which has the power spectrumP S (k )=B[16,17].Thus we stress that we are using a phenomeno-logical power-law spectrum,which does not necessarily follow from any particular inflation model.We shall re-turn to this point later in this paper.After the clear detection of the acoustic peak around ℓ≃200it became evident that the adiabatic modelsfit well to the data[1,2,4,5,18,19].However,this should not be taken as a proof that all pure isocurvature models are ruled out.Some unconventional combination of cosmo-logical parameters,e.g.,Ω=1and a spectrum with a large tilt,could at least in principle give an equally good fit as do the adiabatic models.Pure isocurvature models have two well-recognized problems:excess power at low multipoles and a peak structure that is roughly speaking out of phase byπ/2 when compared to the adiabatic one[20].Since the angu-lar power in the low multipole region was measured quite firmly by the Cosmic Background Explorer(COBE),χ2fitting forces the overall normalization constant in pure isocurvature models to be smaller than in the adiabatic case,which leads to too little power at higher multipoles. The easiest and perhaps the only way to compensate for this is to introduce a large spectral tilt.Moreover,since flat adiabatic modelsfit the observed peak atℓ≃200 well,it is obvious that theℓ≃200peak falls between the first and second peaks of anyflat isocurvature model. Accordingly,in our earlier study[11],the best-fitflat isocurvature model was found to have a largeχ2=116 for30data points and6parameters whereas the best adiabatic model hadχ2=22.Thus we have two possibilities for a better isocurva-ture model.Thefirst is to lower the total energy density parameter so much that the position of thefirst isocur-vature peakfits to the observed peak atℓ≃200,which means that we have to allow for an open universe(Ω<1). The other possibility is to increase the total energy den-sity parameter so much that the position of the second isocurvature peakfits theℓ≃200peak[21],implying a closed universe(Ω>1).In this case thefirst isocurva-ture peak atℓ≃60...100should effectively disappear. In fact,a large spectral tilt would have precisely this ef-fect since it would decrease the relative power at lowℓ. The purpose of the present paper is to study these pos-sibilities systematically tofind out if CDM isocurvature models are indeed completely ruled out by the presently available CMB data.II.METHODS AND RESULTSIn order to compare the isocurvature models with adiabatic ones we choose one representative well-fitted adiabatic model(n adi,Ωm,ΩΛ,ωb,ωc,τ)= (0.98,0.38,0.62,0.021,0.13,0);cf.[1].Using the same data sets and algorithm as for isocurvature models, we getχ2=44for this adiabatic“reference”model. Fig.3(b)confirms that this modelfits well both the low ℓpart of the angular power spectrum and the acoustic peaks.Our starting point for analyzing isocurvature models is a large grid with the following free parameters:•n iso=1.00...7.00(60values)•Ωm=0.06...2.31(16values)•ΩΛ=−1.00...1.10(14values)•ωb=0.001...0.100(10values)•ωc=0.01...1.60(15values),whereΩm is the total matter density,ΩΛis the vacuum energy density,ωb=h2Ωb is the baryon density,andωc= h2Ωc is the CDM density.The sixth free parameter is the overall normalization factor B of Eq.(1).The Hubble constant h is not a free parameter,since h2Ωm=ωm=ωb+ωc.We use a top-hat prior h=0.45...0.90and assumeτ=0for the optical depth due to reionization. The angular power spectrum of all the models in the grid was calculated by CAMB[22]assuming isocurvature CDM initial conditions.We use theχ2method to compare models and data, because it allows us to quickly search a large parameter space.This method is approximate[17]and we do not attempt precise estimates for cosmological parameters or confidence levels.As will be seen,the conclusion is clear enough in ruling out the isocurvature models so that it is not necessary to go to a full maximum likelihood analysis [23].Using the latest Boomerang data[1],together with Maxima-1[3]and COBE data[24]we calculateχ2for each model.The resulting best-χ2contours in the (Ωm,ΩΛ)plane are presented in Fig.1by gray levels. The best-fit model turns out to haveχ2=80with (n iso,Ωm,ΩΛ,ωb,ωc)=(2.00,2.11,−1.00,0.020,1.40). From Fig.1(a)we see that the best-fit isocurvature mod-els lie along two bands in the(Ωm,ΩΛ)plane,the left band corresponding to open universes,and the right cor-responding to closed universes.In the best-fit models the spectral index falls in the range n iso=2...3.A detailed examination of the various pure isocurva-ture models allows us to conclude that the main prob-lems are the spacings of the higher acoustic peaks and the slope in the(lowℓ)Sachs–Wolfe region.COBE mea-sured a close-to-flat Cℓspectrum,but the isocurvature models have a significant positive slope arising from the large primordial blue spectral tilt needed to get enough power at higher multipoles.In the best-fit open models the prominent peak in the CMB data isfitted by thefirst acoustic peak of the isocur-vature model.Fig.1(a)shows that in the best-fit open region thefirst peak lies in the range150<∼ℓ<∼230. Since the data do not show a high second peak,these models need a small baryon densityωb to boost up the first peak and suppress the second peak.(In the adia-batic case,adding more baryons enhances odd acousticnear to the lower right corner.The contours for deviation from the bestfit are as follows:white∆χ2<10;light gray 10<∆χ2<40;medium gray40<∆χ2<100;and dark gray∆χ2>100.(a)Dashed lines show the position(ℓ)of thefirst acoustic peak and solid lines the second peak.(b) Solid lines give the values ofσ8Ω0.56m,and the dotted area is that allowed by the LSS constraint0.43<σ8Ω0.56m<0.70.peaks over even[20],but in the isocurvature case increas-ingωb boosts even peaks.)Actually,all the best-fit open models have a baryon density ofωb=0.001,which is the smallest value in the grid.However,even assuming such an unphysically low baryon density as0.0005only gives about half of the power needed tofit thefirst peak,so not scanning belowωb<0.001seems justified.In the best-fit closed models theℓ≃200peak in the CMB data isfitted by the second isocurvature peak,which lies,according to Fig.1(a),in the range8mχ2=103.The contours for deviation from the bestfit are as follows:white∆χ2<35;light gray35<∆χ2<140;medium gray140<∆χ2<350;and dark gray∆χ2>350.The upper left corner corresponds to the closed models where the second acoustic peakfits the prominent peak in the Cℓdata.(b)The best-fit physical region using thefine grid.The solid contours show the baryon densityωb.The best-fit model hasχ2=121 and the gray levels are as follows:white∆χ2<6;light gray 6<∆χ2<30,medium gray30<∆χ2<60,and dark gray ∆χ2>60.225<∼ℓ<∼265.As one might expect(see,e.g.,[25]for an adiabatic analogy),now the ratio of theℓ≃200peak to the higher multipole Cℓ’s in the datafixesωb near the value0.02in the whole best-fit band.In contrast one ob-tains almost no restriction forωc.This is consistent with Fig.1,whereΩm can be seen to be able to take almost any value,which is then compensated byΩΛto produce the correct peak position.According to Fig.3(a)the best isocurvature model (χ2=80)does badly with the COBE region as well aswith COBE(⋄),Boomerang(•),and Maxima-1(◦)data.(a) Best-fit isocurvature model of Fig.1(solid line)and best-fit open model with LSS constraint(dashed line).(b)Best phys-ical isocurvaturefit from thefine grid(solid line)and the adi-abatic reference model(dashed line).Note that up toℓ=25 theℓaxis is logarithmic.after the prominent peak.This peak isfitted quite well by the second acoustic peak while thefirst acoustic peak appears as a small shoulder aroundℓ≃80.The considerations so far rely on the CMB data only. However,as is well known,when discussing isocurva-ture models it is essential to include also the large-scale structure(LSS)data.As we will see,rough mea-sures are already very effective in constraining the mod-els.Therefore we make use of the the amplitude of the rms massfluctuations in an8h−1Mpc sphere only,de-noted asσ8,which the LSS data restricts to the range0.43<σ8Ω0.56m <0.70[26].The contours ofσ8Ω0.56mareshown in Fig.1(b).Apart from the upper left corner of the(Ωm,ΩΛ)plane,the best-fit closed models appeargive a far too largeσ8Ω0.56m>∼1.5.This is natural, we need a large n iso to do away with thefirst peakisocurvature shoulder”)atℓ≃60...100and to getpower at higher multipoles.A large n iso evidentlyto a largeσ8.To compensate for this,one woulda smallΩm.We have checked that the smallermwe have,the larger n iso is allowed for by the LSS con-In particular,the upper left corner closed models Fig.1b obey the LSS constraint,although they have rather large spectral index n iso≃3.1.On the other hand,the best-fit open models tend toa slightly too smallσ8Ω0.56m.These models have a small n iso 2.1,for the following reasons.(1) these modelsfit thefirst isocurvature peak to the ≃200peak in the data,they do not need a large n iso eliminate thisfirst peak.(2)The smaller scales do not as large a boost from n iso,since power is provided the second peak where the data requires it.Because this smaller n iso these modelsfit the COBE region We have repeated the analysis of minimizingχ2but with the LSS constraint.As one might expect,this most of the best-fit closed models,leaving only with a smallΩm and a largeΩΛ;see the upper leftof Fig.2(a).The reason for this shifting of theclosed-model region to the opposite corner in the m,ΩΛ)plane is easy to rge n iso leadsa largeσ8,and hence the prior0.43<σ8Ω0.56m<0.70Ωm to be small,which in turn implies a largeΛin order to adjust the peak position.After imposing the LSS constraint,the best-fit model no longer a closed one but an open model at the cor-of the parameter space withωb=0.001andΩΛ= 1.00.Thisfit hasχ2=103and(n iso,Ωm,ΩΛ,ωb,ωc)= .05,0.71,−1.00,0.001,0.16).Fig.3(a)shows that the acoustic peak atℓ≃170is too low tofit the data.It is clear that thefit would further improve if one allowed for even smallerωb andΩΛ.However,such a smallωb is in clear conflict with big bang nucleosynthesis(BBN). There is some debate in the BBN community[27]on how small anωb could be acceptable.After imposing a very conservative lower limit,ωb≥0.003,our best-fit open model is already significantly worse than the best-fit closed models.Moreover,the best-fit open models have a very small,even a negative,ΩΛ.This region of the (Ωm,ΩΛ)plane is disfavored by the observed supernova redshift-distance relationship[28].Thus we conclude that the best candidates for pure isocurvature models are the remaining best-fit closed models.These models satisfy the LSS constraint and have an acceptableωb.They lie in the region of smallΩm and largeΩΛ.We scanned this region with afiner grid.The resulting best-χ2contours in the (Ωm,ΩΛ)plane are shown in Fig.2(b)along with the baryon density of these models.The best“physically acceptable”isocurvaturefit has(n iso,Ωm,ΩΛ,ωb,ωc)= (2.80,0.12,0.97,0.015,0.074).Thefit remains very bad, however,withχ2=121for40data points and6pa-rameters,to be compared toχ2=44of theflat adia-batic reference model.Because of the highχ2of the best fit,it is unnecessary to consider the LSS spectrum in a more detailed way.The badness of thefit is mainly due to the COBE and Boomerang data;see Fig.3(b).The COBE contribution toχ2is2.4per COBE data point, the Boomerang contribution is4.2per data point,while the Maxima contribution remains at1.7.The slope of the best-fit model is the reason for the poorfit to COBE,and although the prominent peak in the data isfitted quite well,the“flat adiabatic”peak structure of the second and third peaks in the Boomerang data leads to a con-flict with the isocurvature peak structure.As mentioned earlier,the power-law form for the power spectrum is not necessarily the most natural one in open and closed models due to the effect of spatial curvature. The curvature scale in the models studied is compara-ble to the Hubble scale,or larger.Thus its effect is ex-pected to be reflected in the COBE region of the power spectrum,but not in the Boomerang/Maxima region. To assess the significance of this problem,we repeated our analysis without the COBE data points.The re-sults remained essentially unchanged.Without the8 COBE points we gotχ2=70for the best-fit model,χ2=91for the best-fit with LSS constraint,χ2=89for the best physically acceptablefit from the refined grid, andχ2=40for the adiabatic reference model.Hence the Boomerang data alone are sufficient to rule out pure isocurvature models and our conclusions do not depend on the question of the effect of spatial curvature on the power spectrum.Actually,since the main discriminant is the relative po-sitions of the three peaks in the Boomerang data,which show an“adiabatic”instead of an“isocurvature”pat-tern,our conclusion should be independent of the shape of the primordial power spectrum as long as the observed peaks are indeed due to acoustic oscillations and do not represent features of the primordial power spectrum it-self.III.SUMMARYWe have surveyed a large space of parameters for pure isocurvature models,and allowed for both open and closed universes,tofind out whether there are any pure isocurvature models thatfit the current CMB data better than or at least equally as well as theflat adiabatic model. There are none.We conclude that,even if one ignores the high-z supernova data,pure isocurvature CDM mod-els,including the ones with a heavily tilted spectrum,are completely ruled out by the present CMB and LSS data. Incidentally,the isocurvature models do not do too badly with the Maxima-1data.The main CMB problems are with the COBE and the Boomerang data.To have suffi-cient smaller-scale power,and to suppress thefirst peak and boost the second peak in the closed models,a large blue tilt is needed.This leads to a slope in the Sachs–Wolfe region and reduces the largest-scale power below the level observed by COBE.The most significant prob-lem,however,is with the Boomerang data.Boomerang shows a second and a third peak with a spacing that cor-responds to aflat universe,whereas the position of the first peak in the data cannot befitted byflat isocurvature models.ACKNOWLEDGMENTSThis work was supported by the Academy of Finland under the contracts101-35224and47213.We thank Alessandro Melchiorri for a useful communication,Elina Sihvola for technical help,and the Center for Scientific Computing(Finland)for computational resources.We acknowledge the use of the Code for Anisotropies in the Microwave Background(CAMB)by Antony Lewis and Anthony Challinor.[15]M.Bucher,K.Moodley,and N.Turok,Phys.Rev.D62,083508(2000);astro-ph/0007360.[16]K.M.G´o rski,B.Ratra,R.Stompor,N.Sugiyama,andA.J.Banday,Astrophys.J.Suppl.Ser.114,1,(1998);B.Ratra and P.J.E.Peebles,Phys.Rev.D52,1837(1995); B.Ratra and P.J.E.Peebles,Astrophys.J.Lett.432,L5(1994); D.H.Lyth and A.Woszczyna, Phys.Rev.D52,3338(1995);M.Zaldarriaga,U.Sel-jak,and E.Bertschinger,Astrophys.J.494,491(1998);A. 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Flavoured Large N Gauge Theory in an External Magnetic Field
a r X i v :h e p -t h /0701001v 2 29 J u n 2007Flavoured Large N Gauge Theory in an External Magnetic FieldVeselin G.Filev ⋆,Clifford V.Johnson ⋆,R.C.Rashkov †1and K.S.Viswanathan †⋆Department of Physics and Astronomy,University of Southern California Los Angeles,CA 90089-0484,U.S.A.filev@,johnson1@ †Department of Physics Simon Fraser University and IRMACS Centre Burnaby,BC,V5A 1S6,Canada kviswana@sfu.ca;rash@phys.uni-sofia.bg Abstract We consider a D7-brane probe of AdS 5×S 5in the presence of pure gauge B -field.In the dual gauge theory,the B -field couples to the fundamental matter introduced by the D7-brane and acts as an external magnetic field.The B -field supports a 6-form Ramond-Ramond potential on the D7-branes world volume that breaks the supersymmetry and enables the dual gauge theory to develop a non-zero fermionic condensate.We explore the dependence of the fermionic condensate on the bare quark mass m q and show that at zero bare quark mass a chiral symmetry is spontaneously broken.A study of the meson spectrum reveals a coupling between the vector and scalar modes,and in the limit of weak magnetic field we observe Zeeman splitting of the states.We also observe the characteristic√1On leave from Dept of Physics,Sofia University,Bulgaria.1IntroductionIn recent years,progress has been made in the study of gauge theory with matter in the fundamental representation in the context of gauge/string dualities generalizing the AdS/CFT correspondence.One way to achieve this is by introducing D7-branes in theprobe limit[2]that amounts to the condition N f≪N c.The fundamental strings stretched between the stack of N c D3-branes and the N fflavor D7-branes give rise to N=2hypermul-tiplet.The separation of the D3-and D7-branes in the transverse directions corresponds to the mass of the hypermultiplet,the classical shape of the D7-brane encodes the value of the fermionic condensate,and itsfluctuations describe the light meson spectrum of the theory[3].This technique for introducing fundamental matter has been widely employed in different backgrounds.Of particular interest is the study of non supersymmetric back-grounds and phenomena such as spontaneous chiral symmetry breaking.These phenomena werefirst studied in this context in ref.[4],using analytical and numerical techniques.In several works this approach was further developed,and has proven itself a powerful tool for the exploration of gauge theories,in particular,for the description of their thermodynamic properties or for the building of phenomenological models relevant to QCD[5]–[39].In this paper we will be interested in introducing fundamental matter into the gaugetheory in the presence of an external electromagneticfield that couples to the fundamental fermions.The supersymmetry will be explicitly broken by the externalfield,and we will observe spontaneous symmetry breaking,and non–trivial mixing in the spectrum of mesons.2Fundamental Matter in an External Magnetic Field 2.1Basic ConfigurationLet us consider the AdS5×S5geometry describing the near-horizon physics of a collection of N c extremal D3-branes.ds2=u2u2+R2dΩ25,(1)g s C(4)=u4R2[−dx20+dx21+dx22+dx23]+R2whereρ,ψ,β,γand L,φare polar coordinates in the transverse R4and R2respectively. Note that:u2=ρ2+L2.We use x0,x1,x2,x3,ρ,ψ,β,γto parametrise the world volume of the D7-brane and consider the following ansatz[3]for its embedding:φ≡const,L≡L(ρ),leading to the following form of the induced metric on its worldvolume:d˜s=ρ2+L(ρ)2ρ2+L(ρ)2[(1+L′(ρ)2)dρ2+ρ2dΩ23].(3)Now let us consider the general DBI action:S DBI=−µ7 M8d8ξe−Φ[−det(G ab+B ab+2πα′F ab)]1/2.(4)Hereµ7=[(2π)7α′4]−1is the D7-brane tension,G ab and B ab are the induced metric and B-field on the D7-brane’s world volume,while F ab is its world–volume gaugefield.A simple way to introduce magneticfield would be to consider a pure gauge B-field along parts of the D3-branes’world volume,e.g.:B(2)=Hdx2∧dx3.(5) Since B ab can be mixed with the gaugefield strength F ab,this is equivalent to a magnetic field on the world–volume.Recently a similar approach was used to study drag force in SYM plasma[35].Note that since the B-field is pure gauge,dB=0,the corresponding background is still a solution to the supergravity equations of motion.On the other hand, the gaugefield F ab comes at next order in theα′expansion compared to the metric and the B-field components.Therefore to study the classical embedding of the D-brane one can study only the(G ab+B ab)part of the DBI-action.However,because of the presence of the B-field,there will be terms otfirst order inα′in the full action linear in the gauge field F ab.Hence integrating out F ab will result in a constraint for the classical embedding of the D7-brane.Since for our configuration,we have that:B(2)∧B(2)=0,B(2)∧C(4)=0,and atfirst order inα′the only contribution to the Wess-Zummino is2πα′µ7 F(2)∧C(6).(6) By using the following expansion in the DBI action:[−det(E ab+2πα′F ab)]1/2=√EE ba Fab+O(F2);E=−det E ab;,(7) 2where we have introduced E ab=G ab+B ab as a notation for the generalized induced metric, we obtain the following action tofirst order inα′:S F=πα′µ7EE[ab]F[ab]+2πα′µ7 F(2)∧C(6).(8)The resulting equation of motion does not contain A a and sets the following constraint for the C(6)potential induced by the gauge B-field.g sEE[ba]);a,b,˜µ1,...˜µ6∈M8;.(9)Note that C(6)has a dynamical term proportional to1/κ20in the supergravity action,and that the D7-brane action is proportional toµ7=2π/κ20.Therefore they are at the same order inα′[41].We must solve for C(6)using the action:S C(6)=µ7 B(2)∧C(6)−1−G|dC(6)|2.(10)The solution obtained from equation(10)has to satisfy the constraint given in equation(9). Our next goal will be tofind a consistent ansatz for C(6).To do this let us consider the classical contribution to the DBI action:S NS=−µ7E.(11)From equation(11)one can solve for the classical embedding of the D7-brane,which amounts to second order differential equation for L(ρ)with some appropriate solution L0(ρ).After substituting L0(ρ)in(11)we can extract the form of the C(6)potential induced by the B-field.However one still has to satisfy the constraint(9).It can be verified that with the choice(5)for the B-field and the ansatz of equation(3)for the induced metric,the right-hand side of equation(9)is zero.Then equation(9)and the effective action(10)boil down tofinding a consistent ansatz for C(6)satisfying:∂µ(√πHδ(L−L0(ρ)),(12)or∂µ(√πHδ(L−L0(ρ)),(13)ǫab˜µ1...˜µ6∂a C˜µ1...˜µ6=0;a,b,˜µ1,...˜µ6∈M8;.(14) One can verify that the choice:C(6)01ρψαβ=1is a consistent ansatz and the solution for the C (6)field strength can be found to be:dC (6)L 01ρψαβ=µ7κ20L (ρ2+L 2)2Θ(L −L 0(ρ))sin ψcos ψ.(16)It is this potential which breaks the supersymmety.It is important to note that there is no contradiction between the fact that the B –field that we have chosen does not break the supersymmetry of the AdS 5×S 5supergravity background,on the one hand,and the fact that the physics of the D7–brane probing that background does have supersymmetry broken by the B –field,on the other.This is because the physics of the probe does not back–react on the geometry.In what follows,we will study the physics of the D7-branes and the resulting dual gauge theory physics.Among the solutions for the D7-brane embedding,there will be a class with non-trivial profile having zero asymptotic separation between the D3-and D7-branes.This corresponds to a non-zero fermionic condensate at zero bare quark mass.Therefore the non-zero background magnetic field will spontaneously break the chiral symmetry.Geometrically this corresponds to breaking of the SO (2)rotational symmetry in the (L,φ)-plane [3].2.2Properties of the SolutionWe now proceed with the exploration of the properties of the classical D7-brane embedding.If we consider the action (11)at leading order in α′,we get the following effective lagrangian:L =−µ71+L ′2 (ρ2+L 2)2.(17)The equation of motion for the profile L 0(ρ)of the D7-brane is given by:∂ρ ρ3L ′01+L ′20 (ρ2+L 20)2 + (ρ2+L 20)22ρ3L 0R 4H 2ρ2+ (19)4where the parameters m(the asymptotic separation of the D7-and D3-branes)and c(the degree of bending of the D7-brane)are related to the bare quark mass m q=m/2πα′andthe fermionic condensate ¯ψψ ∝−c respectively[5].As we shall seebelow,the presenceof the external magneticfield and its effect on the dual SYM provide a non vanishing value for the fermionic condensate,furthermore the theory exhibits chiral symmetry breaking.Now notice that H enters in(17)only through the combination H2R4.The other natu-ral scale is the asymptotic separation m.It turns out that different physical configurations can be studied in terms of the ratio˜m2=m2/(HR2):Once the˜m dependence of our solu-tions are known,the m and H dependence follows.Indeed let us introduce dimensionless variables via:ρ=R √H˜L,L′(ρ)=˜L′(˜ρ).(20)The equation of motion(18)then takes the form:∂˜ρ ˜ρ3˜L′1+˜L′2 (˜ρ2+˜L2)2 + (˜ρ2+˜L2)22˜ρ3˜L˜ρ2+...,(22) and using the transformation(20)we can get:c=˜c R3H3/2.(23) It is instructive to studyfirst the properties of(21)for˜m≫1,which corresponds to weak magneticfield H≪m2/R2,or equivalently large quark mass m≫R√(˜ρ2+˜m2)3=0,(24) which has the general solution:η(˜ρ)=C14˜ρ2(˜m2+˜ρ2)+C2.(25)From the definition ofη(˜ρ)and equation(22)we can see that C1=˜c and sinceη|˜ρ→∞=0 we have C2=0.Now if we consider˜m large enough,equation(25)should be valid for all5˜ρ.It turns out that if we require that our solution befinite as˜ρ→0we can determine the large˜m behavior of˜c.Indeed the second term in(25)has the expansion:−˜m4˜m14˜m3+O(˜ρ2).(26)Therefore we deduce that:C1=˜c=14˜m 14˜ρ2(˜m2+˜ρ2).(28)If we go back to dimensionful parameters we can see,using equations(23)and(27)that for weak magneticfield H the theory has developed a fermionic condensate:¯ψψ ∝−c=−R412345m 0.10.2 0.3cm -c crFigure 1:The black line corresponds to (27),one can observe that the analytic result is valid forlarge ˜m .It is also evident that for ˜m =0 ¯ψψ =0.The corresponding value of the condensateis ˜c cr =0.226.ref.[7],where the authors have argued that only the lowest branch of the spiral correspond-ing to positive values of m is the stable one (corresponding to the lowest energy state).The spiral behavior near the origin signals instability of the embedding corresponding to L 0≡0.If we trace the curve of the diagram in figure 3starting from large m ,as we go to smaller values of m we will reach zero bare quark mass for some large negative value of the fermionic condensate c cr .Now if we continue tracing along the diagram one can verify numerically that all other points correspond to embeddings of the D7-brane which inter-sect the D3-brane at least once.(Note also that in ref.[4],such behavior was considered inconsistent with the interpretation of the embedding as a re-normalization group flow.)After further study one finds that the part of the diagram corresponding to negative values of ˜m represents solutions for the D7-brane embedding which intersect the D3-branes odd number of times,while the positive part of the spiral represents solutions which intersect the D3-branes even number of times.The lowest positive branch corresponds to solutions which don’t intersect the D3-branes and is the stable one,while the upper branches have correspondingly 2,4,etc .,intersection points and are ruled out.3Meson Spectrum 3.1General PropertiesWe study the scalar meson spectrum.To do so we will consider quadratic fluctuations [3]of the embedding of the D7-brane in the transverse (L,φ)-plane.It can be shown that because of the diagonal form of the metric the fluctuation modes along the φcoordinate decouple from the one along L .However,because of the non-commutativity introduced72006001000R 2H 200040006000c crFigure 2:A plot of the magnitude of the fermionic condensate at zero bare quark mass c cr asfunction of R 2H ,the black curve represents equation (30). 0.125 0.1 0.075 0.05 0.0250.025m0.2 0.150.10.05cm c cr Figure 3:A magnification of figure 1to show the spiral behavior near the origin of the (−˜c ,˜m )-plane.by the B -field we may expect the scalar fluctuations to couple to the vector fluctuations.This has been observed in ref.[8],where the authors considered the geometric dual to non-commutative super Yang Mills .In our case the mixing will be even stronger,because of the non-trivial profile for the D7-brane embedding,resulting from the broken supersymmetry.Let’s proceed with obtaining the action for the fluctuations.To obtain the contribution from the DBI part of the action we consider the expansion:L =L 0(ρ)+2πα′χ,φ=0+2πα′,(31)where L 0(ρ)is the classical embedding of the D7-brane solution to equation (18).To second order in α′we have the following expression:E ab =E 0ab +2πα′E 1ab +(2πα′)2E 2ab ,(32)8where E0,E1,E2are given by:E0ab=G ab(ρ,L0(ρ),ψ)+B ab,E1ab=R2L0′ρ2+L20 ∂aχ∂bχ+L20∂aΦ∂bΦ −2R2L0L′02∂2L0G abχ2. Here G ab and B ab are the induced metric and Bfield on the D7-brane’s world volume.Now we can substitute equation(33)into equation(11)and expand to second order inα′.It is convenient[8]to introduce the following matrices:||E0ab||−1=S+J,(34) where S is diagonal and J is antisymmetric:||S ab||=diag{−G−111,G−111,G11G211+H2,G−1ρρ,G−1ψψ,G−1αα,G−1ββ},(35)J ab=HR2;Gρρ=R2(1+L′02)ρ2+L20;Gαα=cos2ψGψψ;Gββ=sin2ψGψψ.(37) Now it is straightforward to get the effective action.Atfirst order inα′the action for the scalarfluctuations is thefirst variation of the classical action(11)and is satisfied by the classical equations of motion.The equation of motion for the gaugefield atfirst order was considered in Section2for the computation of the C(6)potential induced by the B-field.Therefore we focus on the second order contribution from the DBI action.After integrating by parts and taking advantage of the Bianchi identities for the gauge field,we end up with the following terms.Forχ:Lχ∝1−E0R21+L′02∂aχ∂bχ+ ∂2L0√−E0L′02χ2,(38)and for F:L F∝1−E0S aa′S bb′F ab F a′b′,(39) and the mixedχ–F terms:L Fχ∝sin2ψand for Φ:L Φ∝1−E 0R 2L 021+L 0′2J 23+J 32∂L 0g (ρ)+2g (ρ)J 23S 22∂L 0G 11,(42)with g (ρ)=√sin ψcos ψ=ρ31+R 4H 22µ7F (2)∧F (2)∧C (4)+(2πα′)µ7F (2)∧B (2)∧˜P[C (4)],(43)where C (4)is the background R-R potential given in equation(1)and ˜C(4)is the pull back of its magnetic dual.One can show that:˜C 4=R 4(ρ2+L 2)2L 2sin ψcos ψdψ∧dα∧dβ∧dφ.(44)Writing φ=2πα′Φwe write for the pull back P [˜C(4)]:P [˜C(4)]=−2πα′2K (ρ)∂a Φdψ∧dα∧dβ∧dx a ,(45)where we have defined:K (ρ)=−R4L 202ρ2+L 02g sd 8ξsin 2ψ2H∂ρK ΦF 01.(48)10Note that this means that only the A 0and A 1components of the gauge field couple to the scalar field Φ.Next the contribution from the first term in (43)is given by:(2πα′)2µ78R 4F ab F cd ǫabcd ,(49)where the indices take values along the ρ,ψ,α,βdirections of the world volume.This will contribute to the equation of motion for A ρ,A ψ,A αand A β,which do not couple to the scalar fluctuations.In this paper we will be interested in analyzing the spectrum of the scalar modes,therefore we will not be interested in the components of the gauge field transverse to the D3-branes world volume.However although there are no sources for these components from the scalar fluctuations,they still couple to the components along the D3-branes as a result setting them to zero will impose constraints on the A 0...A 3.Indeed from the equation of motion for the gauge field along the transverse direction one gets:3a =0S aa ∂b ∂a A a =0,b =ρ,ψ,α,β,(50)(Here,no summation on repeated indices is intended.)However the non-zero B -field ex-plicitly breaks the Lorentz symmetry along the D3-branes’world volume.In particular wehave:S 00=−S 11,S 22=S 33=S 11,(51)which suggests that we should impose:−∂0A 0+∂1A 1=0,∂2A 2+∂3A 3=0.(52)We will see that these constraints are consistent with the equations of motion for A 0...A 3.Indeed with this constraint the equations of motion for χ,Φand A µ,µ=0...3are,for χ:1+L ′02(1+L ′02)2+∆Ω3χ(ρ2+L 20)2 2χ+(53)+1+L ′02∂L 0L ′0∂L 20χ+1+L ′02g∂ρ gL 20∂ρΦρ2+R 4L 20gF 01=0,(54)and finally for A a :11+L ′02+∆Ω3A 0(ρ2+L 20)22A 0+H∂ρK11+L ′02+∆Ω3A 1(ρ2+L 20)22A 1+H∂ρKg∂ρg∂ρA 2(ρ2+L 20)2) +R 4ρ2(1+R 4H 2g∂3χ=0,1(1+L ′02)(1+R 4H 2(ρ2+L 20)2+R 4H22A 3+∆Ω3A 3(ρ2+L 20)2)+f1+R 4H 2g∂ρg∂ρF 01ρ2+R 4g(−∂20+∂21)Φ=0(57)11+L ′02+∆Ω3(−∂0A 0+∂1A 1)(ρ2+L 20)2 2(−∂0A 0+∂1A 1)=0.Note that the first constraint in (52)trivially satisfies the second equation in (57).In thisway we are left with the first equation in (57).Similarly one can show that using the second constraint in (52)the equations of motion in (55)for A 2and A 3boil down to a single equation for F 23:1(1+L ′02)(1+R 4H 2(ρ2+L 20)2+R 4H2 2F 23+∆Ω3F 23(ρ2+L 20)2)+fof the D-brane is known only numerically we have to rely again on numerics to study the meson spectrum.However if we look at equation(18)we can see that the terms responsible for the non–trivial parts of the equation of motion are of order H2.On the other hand, the mixing of the scalar and vector modes due to the term(48)appear atfirst order in H. Therefore it is possible to extract some non-trivial properties of the meson spectrum even at linear order in H and as it turns out,we can observe a Zeeman–like effect:A splitting of states that is proportional to the magnitude of the magneticfield.To describe this,let us study the approximation of weak magneticfield.3.2.1Weak magneticfieldTofirst order in H the classical solution for the D7-brane profile is given by:L0=m+O(H2),(59) where m is the asymptotic separation of the D3and D7-branes and corresponds to the bare quark mass.In this approximation the expressions for g(ρ)and∂ρK(ρ),become:g(ρ)=ρ3,∂ρK(ρ)=4m2R4ρ3ρ3 ρ3m2∂ρΦ +m2∆Ω3(ρ2+m2)22Φ−4H m2R4ρ3∂ρ ρ3∂ρF01 +∆Ω3F01(ρ2+m2)22F01−4H m2R4−∂20+∂21.The resulting equations of motion are:1ρ2φ±+R4(ρ2+m2)3Pφ±=0.(62)Note that P2is the Casimir operator in the(x0,x1)plane only,while2is the Casimir operator along the D3-branes’world volume.If we consider a plane wave e ix.k then we can define:2e ix.k=M2e ix.k,P2e ix.k=M201e ix.k,(63) and we have the relation:M2=M201−k22−k23.(64)13The corresponding spectrum of M 2is continuous in k 2,k 3.However,if we restrict ourselves to motion in the (x 0,x 1)-plane the spectrum is discrete.Indeed let us consider the ansatz:φ±=η±(ρ)e −ix 0k 0+ik 1x 1.(65)Then we can write:1(ρ2+m 2)2M 2±η±∓H4R 4mm 2;¯M ±=R 21+¯M 2±;ǫ=HR 2(1−y )2P ±=0.(68)Next we can expand:P ±=P 0±ǫP 1+O (ǫ2);α±=α0±ǫα1+O (ǫ2);(69)¯M±=¯M 0±ǫα1(4α0+2)α0(α0+1).leading to the following equations for P 0and P 1:y (1−y )P ′′0+2(1−(1−α0)y )P ′0−α0(α0−1)P 0=0,(70)y (1−y )P ′′1+2(1−(1−α0)y )P ′1−α0(α0−1)P 1=(α1(2α0−1)−¯M(n +1)(n +2).14The second equation in (70)isan inhomogeneoushypergeometric equation.However for the ground state,namely n =0,P 0=F (−1,0,2,y )=1and one can easily get the solution:P 1(y )=¯M0y)−¯M0(1−y )α01∓ǫα11−y±ǫ¯M01−y(6α1−¯M0)ln(−y )+16.(75)Now if we require that our solution is regular at y =0and goes as 1/ρ2∝1/y at infinity,the last term in (75)must vanish.Therefore we have:α1=¯M0m .(77)15We observe how the introduction of an external magneticfield breaks the degeneracy of the spectrum given by equation(72)and results in Zeeman splitting of the energy states, proportional to the magnitude of H.Although equation(77)was derived using the ground state it is natural to expect that the same effect takes place for higher excited states.To demonstrate this it is more convenient to employ numerical techniques for solving equation (66)and use the methods described in ref.[4]to extract the spectrum.The resulting plot is presented infigure4.As expected we observe Zeeman splitting of the higher excited states.It is interesting that equation(77)describes well not only the ground state,but also thefirst several excited states.It turns ou that one can easily generalize equation(77)to the case of non-zero mo-mentum in the(x2,x3)-plane.Indeed if we start from equation(62)and proceed with the ansatz:φ±=˜η±(ρ)e−ix.k,(78) we end up with:1M2±˜η±∓H4R4m(ρ2+m2)2M2±+k223;k23≡6 M20.(80) Note that validity of the perturbative analysis suggests thatα1is of the order ofα0and therefore we can trust the above expression as long as k23is of the order of M0.Now it is straightforward to obtain the correction to the spectrum:M±=M0±H1+k223zero.We consider time independent fluctuations satisfying the ansatz e −m 23r 23,(where r 23is the radial coordinate in the (x 2−x 3)-plane).The damping factor in the exponent can be thought of as the mass of the scalar meson in 2Euclidean dimensions.Indeed let us consider the ansatz:Φ=h (ρ)e −ik 2x 2−ik 3x 3Y l (S 3),(82)where Y l (S 3)are the spherical harmonics on the S 3sphere satisfying:∆Ω3Y l =−l (l +2)Y l .With this set-up the equation of motion for Φ,equation (54),reduces to equation for h (ρ):11+L ′02−L 20l (l +2)(ρ2+L 20)2+R 4H 2h (ρ)=0,(83)where we have defined:m 223=−k 22−k 23.(84)Before we proceed with the numerical analysis of equation (83)let us introduce dimension-less variables by performing the transformation (20)and defining:˜m 23=RH m 23.(85)The resulting equation is:˜ρ2+˜L21+˜L ′2(1+(˜ρ2+˜L2)2)1/2∂˜ρ˜ρ3 1+1√˜ρ2l (l +2)h (˜ρ)+˜L 2˜m 223R 2Hwe observe ∝√0.511.522.53m2468m 23Figure 5:Spectrum of ˜m 23vs.˜m .The dashed line represents the lowest level of the mesonspectrum for pure AdS 5×S 5space0.00250.0050.00750.010.01250.0150.0175m0.10.20.30.4m23Figure 6:Enlargement of part of the spectrum of ˜m 23vs ˜m fromfigure5.The black solid curve shows the ∝√˜m behavior plotted in figure 6,while the excited states tend to some finite values at zero bare quark mass.The n =0states merge into the Goldstone boson of the spontaneously broken chiral symmetry.180.51 1.52 2.5351015202530 23n 3n 2n 4n 1n 0Figure 7:Spectrum of ˜m 23vs ˜m for n =0...4.The dashed lines represent the spectrum forAdS 5×S 5space.4AcknowledgmentsV.G.Filev would like to thank T.Albash,I.Bars,A.Kundu,R.Myers and N.Warner for useful discussions and comments.The research of C.V.Johnson and V.G.Filev was supported in part by the US Department of Energy.We would specially like to thank Rene Meyer and Karl Landsteiner for commenting on the first version of the paper.The research of K.S.Viswanatan and R.C.Rashkov has been partially supported by an operating grant from NSERC and Bulgarian NSF BUF-14/06.R.C.Rashkov and V.G.Filev thank Department of Physics and IRMACS for hospitality at the final stage of this project.19References[1]O.Aharony,S.S.Gubser,J.M.Maldacena,H.Ooguri and Y.Oz,Phys.Rept.323,183(2000)[arXiv:hep-th/9905111].[2]A.Karch and E.Katz,JHEP0206,043(2002)[arXiv:hep-th/0205236].[3]M.Kruczenski,D.Mateos,R.C.Myers,and D.J.Winters,“Meson spectroscopy inAdS/CFT withflavour,”JHEP07(2003)049,[4]J.Babington,J.Erdmenger,N.J.Evans,Z.Guralnik and I.Kirsch,“Chiral symmetrybreaking and pions in non-supersymmetric gauge/gravity Phys.Rev.D69,066007 (2004)[arXiv:hep-th/0306018].[5]M.Kruczenski,D.Mateos,R.C.Myers and D.J.Winters,JHEP0405,041(2004)[arXiv:hep-th/0311270].[6]T.Albash,V.Filev,C.V.Johnson and 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2 We conclude in Sec. V.
II. MAGNETIC NEUTRON SCATTERING
G. Seibold
Institut f¨ ur Physik, BTU Cottbus, PBox 101344, 03013 Cottbus, Germany
arXiv:cond-mat/0507131v1 [cond-mat.str-el] 6 Jul 2005
R. Coldea
Oxford Physics, Clarendon Laboratory, Oxford OX1 3PU, United Kingdom (Dated: February 2, 2008) We present estimates in the Hubbard and Heisenberg models for the spectral weight in magnetic neutron scattering experiments on the cuprates. With the aid of spin-wave theory and the time dependent Gutzwiller approximation we discuss how the spectral weight is distributed among the different channels and between high and low energies. In addition to the well known total moment sum rule we discuss sum rules for each component of the dynamical structure factor tensor which are peculiar for spin 1/2 systems. The various factors that reduce the spectral weight at the relevant energies are singled out and analyzed like: shielding factors, weight at electronic energies, multimagnon process etc. Although about 10% ∼ 15% of the naively expected weight is detected in experiments after consideration of these factors the missing weight is within the experimental uncertainties. A large fraction of the spectral weight is hard to detect with present experimental conditions.
day experimental conditions. Theoretical estimates are performed in the antiferromagnetic (AFM) phase using the Heisenberg and the Hubbard model combining spinwave theory, numerical results and the time dependent Gutzwiller approximation (TDGA)7,8,9 and in the doped phase in the Hubbard model within the TDGA. Apart from the mentioned 1 − x factor we discuss the so called “shielding factors” due to an incomplete formation of magnetic moments. We estimate the spectral weight loss to electronic transitions at energies too high to be detectable by present day inelastic magnetic neutron scattering experiments and also the weight in multimagnon processes which is either at too high energies or is so broad in energy and momentum that it is not detectable in unpolarized neutron scattering experiments. After consideration of all these factors we arrive to the conclusion that within the experimental uncertainties the sum rule is not violated (which is reassuring) on the other hand a major fraction of the spectral weight is very hard to detect with present experimental conditions. The outline of the paper is at follows. In Sec. II we shortly review the theory of magnetic neutron scattering and the relevant sum rules to fix notations. This section has also a pedagogical character. Apart from the well known total moment sum rule we discuss sum rules for each component of the dynamical structure factor tensor which, to the best of our knowledge, have not been applied in the present context. We also highlight some simple experimental facts that are usually assumed as granted in experimental works, like domain averages (Sec. II C), but often overlooked in theoretical works. In Sec. III we discuss the spectral weight distribution in the undoped case and in Sec. IV we discuss the doped case.
Where is the spectral weight in magnetic neutron scattering in the cuprates?
J. Lorenzana
SMC-INFM, ISC-CNR, Dipartimento di Fisica, Universit` a di Roma La Sapienza, P. Aldo Moro 2, 00185 Roma, Italy
PACS numbers: 74.25.Ha 78.70.Nx 71.10INTRODUCTION
Magnetic neutron scattering (MNS) in high temperature superconducting cuprates usually detects about 10% ∼ 15% of the spectral weight dictated by a naive application of sum rules. For example the total weight in a wide range of energy and momentum in a recent experiment1 in La2−x Bax CuO4 , with x = 0.125, is ∼ 0.22µ2 B whereas in the insulating phase the naive expectation from sum rules is that one should find 2µ2 B . It is usually argued that this value should be corrected for the hole destruction of moments by a 1 − x factor which still leaves a large fraction of spectral weight undetected. This rises various problems in the interpretation of MNS. For example it has been argued that the average of the dynamical susceptibility weighted by the Fourier transform of the magnetic interaction can be used to estimate the energy involved in magnetic pairing and its temperature dependence.2,3,4,5,6 Clearly to obtain an absolute estimate the spectral weight problem needs to be sorted out first. Furthermore modeling the dynamical structure factor probed by MNS becomes rather problematic since sensible theoretical models do satisfy sum rules. Indeed any theoretical claim of intensity agreement with the measured dynamical structure factor in absolute units needs to explain how the sum rule is satisfied or why it is violated. This is even more stringent in spin only models for which neither 1 − x factors nor shielding corrections apply. The purpose of this work is to explain this apparent discrepancy. We provide theoretical estimates of the various factors which correct the sum rule and estimate what fraction of the spectral weight is accessible to present