暴涨宇宙学与暗能量[001]
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• 微波背景辐射（CMB）
Wilkinson Microwave Anisotropy Probe (WMAP) Observations
Balloon Observations Of Millimetric Extragalactic Radiation And Geophysics
• 大尺度结构（LSS）
1033 eV
m 2 M pl
If yes, very interesting: 2 of the biggest discoveries in the recent years Predictions : neutrino masses vary and cosmological CPT violation
Solution:
Q 3
4 10(2
4)
g1 / 2T 2
nB
/
s
0.01c
T M
Cosmological CPT Violation
Dark Matter Detection EGRET
Based on local cosmic ray spectrum gives consistent gamma ray spectrum in 30 MeV~500 MeV, above 1 GeV there is an excess.
Cosmology and Collider Physics
中科院高能所 张新民
2006.10.28
John C. Mather NASA Goddard Space Flight Center, Greenbelt, MD, USA, George F. Smoot University of California, Berkeley, CA, USA
两种产生机制： 1. 热产生 （像光子退耦一样） 2. 非热产生
Dark Matter Detection
There are great progress in dark matter direct detection. New experiments are going to take data.
"for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation".
Cosmic Background Explorer (COBE) achievements:
Sakharov 三条件: A.D. Sakharov, JETP Lett. 5, 24 (1967).
1. 重子数破坏 2. C 和 CP 破坏 3. 脱离热平衡
Leptogenesis
M. Fukugita and T. Yanagida, Phys. Lett. B 174, 45 (1986); P. Langacker, R.D Peccei, and T. Yanagida, Mod. Phys.Lett.A 1,541 (1986); M.A. Luty, Phys. Rev. D 45, 455 (1992); R.N. Mohapatra and X. Zhang, Phys. Rev. D 45, 2688 (1992).
nB
nb nb
gb
2 2
E(E2
m
1/ 2
m2)
dE
[1 1exp[(E
)
/
T
]
] 1
1exp[(E ) /T ]
nB
c
gbQ T 2 6M
宇宙熵密度：
s
2 2
45
gT 3
nB / s
15c
4 2
gbQ gMT
观测值：
nB / s 10 10
模型： V (Q) f (Q)Exp[( / M Planck )Q]
Inflation：什么是inflaton？
暗物质粒子最佳候选者： 轴子(Axion) 中性伴随子（Neutralino）
近年，较多研究“温暗物质”： Interacting Dark Matter Non-thermal produced Neutralino Steril Neutrino Gravitino Quintessino
1. 右手中微子的 Majorana 质量项破坏轻子数 2. 右手中微子的 Yukawa 耦合项破坏 C 和 CP 3. 右手中微子脱离热平衡
Sphaleron 过程将部分轻子数转化为重子数
V.A. Kuzmin, V.A. Rubakov and M.E. Shaposhnikov, Phys. Lett. B 155, 36 (1985).
I. 宇宙学参数
暗能量模型：
Primordial power spectrum:
Dark Energy equation of state:
II. 天文观测数据： • 超新星（SN）
High Z Search Team (Riess et al. 2004) Supernova Legacy Survey (SNLS)
Solar Neutrino oscillation ：
i
d dr
e
1 2E
U
(m10 (M
M 1 (r ))2 3 (r))2
(M 3 (r))2 (m20 M 2 (r))2
U
A(r ) 0
0 0
e
D.B. Kaplan et al., PRL 93,091801 (2003);
V. Barger et al., hep-ph/0502196;
I. Some astrophysics observations can not be explained by the canonical physics. They may indicate the signal of DM, however, no conclusion can be drawn now.
M. Cirelli et al., hep-ph/0503028.
Studying Dark Energy with LAMOST
LAMOST的效果图
Baryo/Leptogenesis 机制
正反物质不对称：
M. Tegmark et al, Phys.Rev. D 69, 103501 (2004).
1. The CMB shape (Black body spectrum); 2. Detect the temperature fluctuation (~10-5).
Precision Cosmology
SN, Maxima, Boomerang, DASI, WMAP, SDSS, 2dfGRS, “Golden Sample”, SNLS
粒子宇宙学研究进展
•暗物质粒子探测
•暗能量模型
•Baryogenesis andwk.baidu.comTop Quark Physics
需要新物理
暗物质：中微子是暗物质，但不是冷暗物 质；什么是冷暗物质？
暗能量：势能和真空能是暗能量，但理论 预言太大－宇宙学常数问题？
反物质：标准模型可以产生正反物质不对 称，但太小，需要新物理？
The last result is given by CDMS. The null result give stronger constraints on the SUSY parameters. The DAMA region is almost entirely excluded.
Dark Matter Detection
暗能量
基本特征：
a/ a 4G ( 3 p)
3
a 0 3p 0 w p / 1/ 3
注意：辐射 w=1/3, 物质 w=0
1. 真空能： w=-1 (宇宙学常数问题) 2. Quintessence: -1≤w≤1
精质
3. Phantom: -1≥w
幽灵
4. Quintom: w transit from below –1 to above -1
C.S. Li, Z.G. Si, ......
一个统一描述 DE 和 B 的模型
问题的提出： Dirac 理论
反粒子 －－－－Baryogenesis “真空不空” －－－－ Dark Energy
微观
宇观
Any connections?
Lint
c Q M
J
B
重子有效化学势
热平衡
Need new physics for baryogenesis
Different approaches to new physics 1) SUSY 2) Multi-Higgs 3) Left-right symmetric model 4) Extra dimension 5) Effective lagrangian -- anomalous couplings
COBE
Inflation + Dark Matter + Dark Energy + Particle Physics
WMAP
Questions:
1. Inflation mechanism ... ? 2. Dark Matter Particle ... ? 3. Properties of Dark Energy ... ? 4. How to generate the matter and anti-matter asymmetry ... ?
Taking the contribution from dark matter annihilation into account the data can be well explained.
Detection of Dark Matter in China
I. Yang BaJing
II. Quintessino Heavy long-lived charged particle
精灵
暗能量场：宇宙空间中的“以太”
QF F 精细结构常数的改变
Quintom ??
Dark Energy and neutrinos：
Any connection between Dark Energy and neutrinos?
1. ΛCDM: (103ev)4 (m )4
2. QCDM: mQ
Q ll
M
QN
c R
N
R
m
Xinmin Zhang etal. PRD68, 087301 (2003)
Neutrino oscillation probes of Dark Energy
Basic idea：meff ( ) m0 M ( )
given by Veff ()
Veff ( ) V ( ) i ( ) i ,e, p, n
II. One of such experiments is the HEAT. There is an excess above 8 GeV, which can be explained by dark matter annihilation.
III. Sensitivity will be greatly improved at Pamela and AMS02.
Outline of the talk
Current Status on Cosmology; Baryogenesis and collider physics; Cosmological CPT violation and its test with CMB; Summary
宇宙学模型及其检验
轴子(Axion)
为解决强CP破坏问题而引进 (Peccei & Quinn)
g
2 s
32
a~a G a
( 10 9 ?)
轴子: 标量粒子
ma
~
2QCD f PQ
~ 103 eV
探测:
至今未发现
WIMP(弱作用重粒子)
例如，超对称模型中的中性伴随子(neutralino).
Picture of DM distribution at the galaxy
Sloan Digital Sky Survey (SDSS) Two degree Field Galaxy Redshift Survey
III. 数据拟和分析：
Monte Carlo Markov Chains 上海超级计算机
创新点：暗能量扰动
Results
No questions about the existence of Dark Matter and Dark Energy
Wilkinson Microwave Anisotropy Probe (WMAP) Observations
Balloon Observations Of Millimetric Extragalactic Radiation And Geophysics
• 大尺度结构（LSS）
1033 eV
m 2 M pl
If yes, very interesting: 2 of the biggest discoveries in the recent years Predictions : neutrino masses vary and cosmological CPT violation
Solution:
Q 3
4 10(2
4)
g1 / 2T 2
nB
/
s
0.01c
T M
Cosmological CPT Violation
Dark Matter Detection EGRET
Based on local cosmic ray spectrum gives consistent gamma ray spectrum in 30 MeV~500 MeV, above 1 GeV there is an excess.
Cosmology and Collider Physics
中科院高能所 张新民
2006.10.28
John C. Mather NASA Goddard Space Flight Center, Greenbelt, MD, USA, George F. Smoot University of California, Berkeley, CA, USA
两种产生机制： 1. 热产生 （像光子退耦一样） 2. 非热产生
Dark Matter Detection
There are great progress in dark matter direct detection. New experiments are going to take data.
"for their discovery of the blackbody form and anisotropy of the cosmic microwave background radiation".
Cosmic Background Explorer (COBE) achievements:
Sakharov 三条件: A.D. Sakharov, JETP Lett. 5, 24 (1967).
1. 重子数破坏 2. C 和 CP 破坏 3. 脱离热平衡
Leptogenesis
M. Fukugita and T. Yanagida, Phys. Lett. B 174, 45 (1986); P. Langacker, R.D Peccei, and T. Yanagida, Mod. Phys.Lett.A 1,541 (1986); M.A. Luty, Phys. Rev. D 45, 455 (1992); R.N. Mohapatra and X. Zhang, Phys. Rev. D 45, 2688 (1992).
nB
nb nb
gb
2 2
E(E2
m
1/ 2
m2)
dE
[1 1exp[(E
)
/
T
]
] 1
1exp[(E ) /T ]
nB
c
gbQ T 2 6M
宇宙熵密度：
s
2 2
45
gT 3
nB / s
15c
4 2
gbQ gMT
观测值：
nB / s 10 10
模型： V (Q) f (Q)Exp[( / M Planck )Q]
Inflation：什么是inflaton？
暗物质粒子最佳候选者： 轴子(Axion) 中性伴随子（Neutralino）
近年，较多研究“温暗物质”： Interacting Dark Matter Non-thermal produced Neutralino Steril Neutrino Gravitino Quintessino
1. 右手中微子的 Majorana 质量项破坏轻子数 2. 右手中微子的 Yukawa 耦合项破坏 C 和 CP 3. 右手中微子脱离热平衡
Sphaleron 过程将部分轻子数转化为重子数
V.A. Kuzmin, V.A. Rubakov and M.E. Shaposhnikov, Phys. Lett. B 155, 36 (1985).
I. 宇宙学参数
暗能量模型：
Primordial power spectrum:
Dark Energy equation of state:
II. 天文观测数据： • 超新星（SN）
High Z Search Team (Riess et al. 2004) Supernova Legacy Survey (SNLS)
Solar Neutrino oscillation ：
i
d dr
e
1 2E
U
(m10 (M
M 1 (r ))2 3 (r))2
(M 3 (r))2 (m20 M 2 (r))2
U
A(r ) 0
0 0
e
D.B. Kaplan et al., PRL 93,091801 (2003);
V. Barger et al., hep-ph/0502196;
I. Some astrophysics observations can not be explained by the canonical physics. They may indicate the signal of DM, however, no conclusion can be drawn now.
M. Cirelli et al., hep-ph/0503028.
Studying Dark Energy with LAMOST
LAMOST的效果图
Baryo/Leptogenesis 机制
正反物质不对称：
M. Tegmark et al, Phys.Rev. D 69, 103501 (2004).
1. The CMB shape (Black body spectrum); 2. Detect the temperature fluctuation (~10-5).
Precision Cosmology
SN, Maxima, Boomerang, DASI, WMAP, SDSS, 2dfGRS, “Golden Sample”, SNLS
粒子宇宙学研究进展
•暗物质粒子探测
•暗能量模型
•Baryogenesis andwk.baidu.comTop Quark Physics
需要新物理
暗物质：中微子是暗物质，但不是冷暗物 质；什么是冷暗物质？
暗能量：势能和真空能是暗能量，但理论 预言太大－宇宙学常数问题？
反物质：标准模型可以产生正反物质不对 称，但太小，需要新物理？
The last result is given by CDMS. The null result give stronger constraints on the SUSY parameters. The DAMA region is almost entirely excluded.
Dark Matter Detection
暗能量
基本特征：
a/ a 4G ( 3 p)
3
a 0 3p 0 w p / 1/ 3
注意：辐射 w=1/3, 物质 w=0
1. 真空能： w=-1 (宇宙学常数问题) 2. Quintessence: -1≤w≤1
精质
3. Phantom: -1≥w
幽灵
4. Quintom: w transit from below –1 to above -1
C.S. Li, Z.G. Si, ......
一个统一描述 DE 和 B 的模型
问题的提出： Dirac 理论
反粒子 －－－－Baryogenesis “真空不空” －－－－ Dark Energy
微观
宇观
Any connections?
Lint
c Q M
J
B
重子有效化学势
热平衡
Need new physics for baryogenesis
Different approaches to new physics 1) SUSY 2) Multi-Higgs 3) Left-right symmetric model 4) Extra dimension 5) Effective lagrangian -- anomalous couplings
COBE
Inflation + Dark Matter + Dark Energy + Particle Physics
WMAP
Questions:
1. Inflation mechanism ... ? 2. Dark Matter Particle ... ? 3. Properties of Dark Energy ... ? 4. How to generate the matter and anti-matter asymmetry ... ?
Taking the contribution from dark matter annihilation into account the data can be well explained.
Detection of Dark Matter in China
I. Yang BaJing
II. Quintessino Heavy long-lived charged particle
精灵
暗能量场：宇宙空间中的“以太”
QF F 精细结构常数的改变
Quintom ??
Dark Energy and neutrinos：
Any connection between Dark Energy and neutrinos?
1. ΛCDM: (103ev)4 (m )4
2. QCDM: mQ
Q ll
M
QN
c R
N
R
m
Xinmin Zhang etal. PRD68, 087301 (2003)
Neutrino oscillation probes of Dark Energy
Basic idea：meff ( ) m0 M ( )
given by Veff ()
Veff ( ) V ( ) i ( ) i ,e, p, n
II. One of such experiments is the HEAT. There is an excess above 8 GeV, which can be explained by dark matter annihilation.
III. Sensitivity will be greatly improved at Pamela and AMS02.
Outline of the talk
Current Status on Cosmology; Baryogenesis and collider physics; Cosmological CPT violation and its test with CMB; Summary
宇宙学模型及其检验
轴子(Axion)
为解决强CP破坏问题而引进 (Peccei & Quinn)
g
2 s
32
a~a G a
( 10 9 ?)
轴子: 标量粒子
ma
~
2QCD f PQ
~ 103 eV
探测:
至今未发现
WIMP(弱作用重粒子)
例如，超对称模型中的中性伴随子(neutralino).
Picture of DM distribution at the galaxy
Sloan Digital Sky Survey (SDSS) Two degree Field Galaxy Redshift Survey
III. 数据拟和分析：
Monte Carlo Markov Chains 上海超级计算机
创新点：暗能量扰动
Results
No questions about the existence of Dark Matter and Dark Energy