SEARCH FOR EXCITED FERMIONS AT HERA H1 Collaboration

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和宇航员对话想问的问题小学英语作文

和宇航员对话想问的问题小学英语作文

和宇航员对话想问的问题小学英语作文全文共6篇示例,供读者参考篇1Questions I'd Like to Ask an AstronautEver since I was a little kid, I've been fascinated by space and the idea of exploring the unknown vastness that lies beyond our planet. The thought of venturing out into the cosmos, leaving Earth's cozy embrace, and experiencing the wonders of the universe firsthand is both thrilling and daunting. If given the chance to have a conversation with an astronaut, there are so many questions I would love to ask them.First and foremost, I would inquire about their journey to becoming an astronaut. What inspired them to pursue this extraordinary career path? Was it a lifelong dream, or did the passion develop later in life? I'd be curious to learn about the rigorous training process they underwent, the challenges they faced, and the sacrifices they had to make along the way. Becoming an astronaut is no easy feat, and I'd love to gain insight into the dedication and perseverance required to achieve such a lofty goal.Next, I would ask them to describe the experience of liftoff and the moments leading up to it. Can they even put into words the mixture of excitement, fear, and anticipation they must have felt as the countdown reached zero and the powerful rockets ignited beneath them? I imagine the sheer force and magnitude of the launch must be utterly indescribable. I'd love to hear their personal accounts of those heart-pounding moments when they left Earth's embrace and embarked on their cosmic voyage.Once in space, the questions would only multiply. What was their first impression upon gazing at our beautiful, blue planet from afar? Did it fill them with a newfound appreciation for the fragility and preciousness of our world? I'd be curious to know if the experience of seeing Earth from such a unique vantage point changed their perspective on life or instilled a deeper sense of responsibility towards protecting our planet.I would also inquire about the challenges of living and working in the microgravity environment of space. How did they adapt to the absence of gravity, and what tasks or everyday activities proved to be the most difficult? Did they experience any unexpected physical or psychological effects during their time in space? Understanding the realities of life in such an alien environment would be fascinating.Inevitably, the conversation would turn to the future of space exploration and the role humans might play in it. I'd ask for their thoughts on the potential for long-term human habitation on other planets or moons, such as Mars or the lunar surface. What challenges and obstacles would need to be overcome to make such endeavors possible? And what would be the broader implications and benefits for humanity if we were to establish a permanent presence beyond Earth?Furthermore, I'd be curious to hear their perspectives on the search for extraterrestrial life. Do they believe we are alone in the universe, or is the existence of other intelligent life forms a real possibility? If alien life were discovered, what might that mean for our understanding of the cosmos and our place within it?Beyond the scientific and technological aspects, I would also inquire about the personal and emotional impact of their experiences in space. Did the breathtaking vistas and the vastness of the universe instill a sense of humility or insignificance? Or did it perhaps reinforce the idea that篇2Questions I'd Love to Ask an AstronautEver since I was a little kid, I've been fascinated by space exploration and astronauts. I used to stare up at the night sky in awe, imagining what it would be like to float weightlessly among the stars. Astronauts are like real-life superheroes to me - brave men and women who venture into the unknown depths of the cosmos.If I ever got the chance to talk to an astronaut, there are so many questions I would ask them. I've tried to imagine what their incredible experiences must be like, but I'm sure the reality is far beyond what I can even picture in my mind.First off, I would ask them what it felt like when they first left the Earth's atmosphere and saw our beautiful planet from space. Did it take their breath away? Did they feel a sense of wonder at how tiny and fragile Earth looks from that vantage point? I've seen the amazing photos, but I can only imagine howmind-blowing it must be to witness that view with your own eyes.Speaking of photos, I'd love to know what it's like to look out into the inky blackness of space and see stars and galaxies that we can barely make out from Earth with our best telescopes. Is it as breathtaking as it seems, or do astronauts almost take thatincredible view for granted after a while since it's part of their daily routine in space?I'm also super curious about what the experience of being in a rocket during launch feels like. Is it terrifying, exhilarating, or a mixture of both? Do astronauts get intense adrenaline rushes or does their training help them stay calm through all those intense g-forces? I can't even fathom what it must feel like to be strapped into a rocket and then blasted off into the sky.Another thing I've always wondered about is how astronauts adapt to living in zero gravity conditions for extended periods. Is it really disorienting at first, or do they get used to it quickly? What's it like to be able to float around freely instead of being weighed down by gravity? I imagine even simple tasks like eating and drinking must be totally different experiences.I'd be really eager to learn about the day-to-day routines and schedules that astronauts follow on long space missions. How do they balance work responsibilities with personal time and rest? Do they get opportunities to do fun activities like watch movies or read books? Or does the sheer wonder of being in space trump the need for typical entertainment?On a more serious note, I'm really interested in learning about the vital scientific research and experiments astronautsconduct while in space. Whether it's studying things like radiation's effects on the human body or unlocking mysteries about the formation of the universe, their work is crucial to expanding our knowledge. I'd ask what types of studies they're working on and how those further humanity's understanding of our place in the cosmos.Another thing I'm dying to know is what astronauts enjoy the most about being in space, and what are the biggest challenges or things they struggle with. Is the exhilarating feeling of weightlessness addictive, or do they end up missing gravity after a while? What's the hardest part about being confined to a relatively small space station for months at a time? I imagine being an astronaut takes an immense mental and physical toll, in addition to all the rewards.I'd probably have to fight back happy tears if I got to ask astronauts what their most awe-inspiring or profound moments have been while in space. Whether it's witnessing a spectacular cosmic event, enjoying a deepened appreciation for our planet, or just being floored by the majesty of the universe around them, I'm sure they must have experiences that change their perspectives forever. Those stories could be life-changing for us Earthlings to hear.Finally, I might ask if spending time in space and seeing Earth from that ultra-rare vantage point has affected their philosophies or ways of looking at life. Does being an astronaut fundamentally transform a person's worldview or make them think about our existence in新的ways? I'd be honored to gain that type of perspective and insight.Those are just a few of the bajillion questions I'd love to ask an astronaut if given the chance. While I'll probably never get to experience space exploration myself, I'll always be in awe of those who do. Talking to a real-life spacefarer would be a dream come true and one of the coolest experiences imaginable for us starry-eyed Earth kids. Astronauts are篇3Questions I'd Love to Ask an AstronautEver since I was a little kid, I've been fascinated by space and the idea of exploring the unknown vastness that lies beyond our Earth. The thought of venturing into the great cosmic frontier has always filled me with a sense of wonder and excitement. And who better to learn about this incredible journey than from the brave men and women who have actually experienced it firsthand – the astronauts?If I ever had the chance to meet and chat with an astronaut, there are so many questions I'd love to ask them. First and foremost, I'd be curious to know what inspired them to pursue this extraordinary career path. Was it a lifelong dream or a passion that developed later in life? What motivated them to take on such a daring and challenging profession?I'd also be eager to learn about the rigorous training process they had to undergo. How did they prepare both physically and mentally for the harsh conditions of space travel? What were some of the most difficult or grueling aspects of their training? And how did they cope with the immense stress and pressure that must have accompanied such intense preparation?I'd want to know about the challenges and difficulties they faced during their missions. Were there ever any harrowing moments or close calls that tested their resolve and training? How did they handle the intense confinement of living and working in such a small space for extended periods? And what was it like to perform complex tasks and experiments in the unique environment of zero gravity?Naturally, I'd be incredibly curious about the sights and experiences that left the most lasting impressions on them. What was the most breathtaking celestial phenomenon they witnessed?Did they have any profound or life-changing realizations while gazing down at our fragile planet from above? And were there any humorous or lighthearted moments that helped break the tension or monotony of their missions?Beyond the personal experiences, I'd be eager to pick their brains about the broader implications and future of space exploration. What do they see as the most promising avenues for future research and discovery? Do they believe manned missions to other planets or even beyond our solar system could become a reality in our lifetimes? And what role do they think the private sector and commercial space industry might play in driving these endeavors forward?As someone who has spent countless hours gazing up at the night sky and dreaming of the wonders that lie among the stars, the opportunity to speak with an astronaut would be an absolute dream come true. Their firsthand experiences and insights would not only satisfy my boundless curiosity but also provide invaluable inspiration and guidance for anyone aspiring to follow in their footsteps.While the chances of such an encounter may be slim, I can't help but imagine the captivating stories and incredible tales an astronaut would have to share. From the breathtaking beauty ofEarth suspended in the inky blackness of space to the challenges and triumphs of exploring the great unknown, their perspectives and wisdom would undoubtedly leave a lasting impact on my life and further fuel my passion for space exploration.So, to any astronauts out there reading this, know that there are countless dreamers and stargazers like myself who would jump at the chance to pick your brains and learn from your extraordinary experiences. Your journeys have not only expanded the boundaries of human knowledge but also captured the imagination of countless people around the world. And for that, we are forever grateful and in awe of your bravery and accomplishments.篇4Talking to an Astronaut: My List of QuestionsEver since I was a little kid, I've been fascinated by space. I have a telescope that I use to gaze up at the stars and planets on clear nights. I read every book about space I can get my hands on from the library. And my biggest dream is to become an astronaut someday and travel to the Moon or even Mars!That's why I was so excited when my teacher told our class that we would have a very special visitor coming to speak with us- a real astronaut who has actually been to space! I could hardly sit still thinking about all the questions I would ask. After lots of thought, here is my list of questions I hope to ask the astronaut when they visit:What is it like to launch into space aboard the rocket? I've seen videos of rocket launches and it looks both terrifying with all that fire and shaking, but also amazing as you blast off the ground. Does it feel as intense as it looks? Are you strapped in very tightly?Once you get into space, what does it feel like being in zero gravity and floating around? Does it make you feel dizzy or sick at first not having any up or down? Or is it fun to push off and float wherever you want? I've heard some astronauts have a hard time at first until they get their "space legs."How do you go to the bathroom in space? This might seem like a silly question, but I'm really curious! Is it difficult having to go to the bathroom while floating around? Do you have to be strapped into a special toilet? I've heard astronauts have to be really careful or it could be a mess!What is your daily routine like on a space mission? Do you have set times to wake up, exercise, eat meals, do experiments, etc? Or is it more of a go-with-the-flow situation since you're in adifferent environment? I imagine it's really different from normal life on Earth.What is your favorite space food to eat? I've seen videos of astronauts squeezing food out of tubes and adding water to rehydrate freeze-dried ice cream and snacks. Does the food taste pretty good or is it more to just get nutrition? Do you get tired of eating the same things over and over?How do you stay entertained during long stretches of time in the spacecraft? Do you watch movies, read books, play games with your crewmates? I can't imagine how I'd stay occupied being confined to such a small space for weeks or months at a time. I'd probably go stir crazy!What does the Earth look like from space? I've seen beautiful pictures of the Earth from the International Space Station, but I wonder how it appears with your own eyes in person seeing our whole planet floating in the blackness of space. Is it breathtaking or does it start to look normal after a while?What training did you have to go through to become an astronaut? I know it's extremely competitive and difficult, with lots of tests of your mental and physical abilities. Did you have to practice living in simulations of space conditions? Learn all kindsof science and technical skills? I'll have to work really hard if I want that job someday!What is your favorite or most amazing experience you had during a spaceflight? Seeing a sunrise from orbit? Doing a spacewalk? Watching a rocket launch from space? I can only imagine how incredible everything must look and feel so different from anything on Earth.What advice would you give a kid like me who dreams of becoming an astronaut? Besides working hard in school at all my science and math classes, what should I be doing now to help achieve that goal? Read certain books? Attend space camps? Look into special programs or internships? I'll do whatever it takes!I have so many other questions too, like what the re-entry through the atmosphere feels like, what items you wish you had brought with you, seeing other planets and stars up close, and so on. But those are my top 10 burning questions for now that I'm hoping to ask the astronaut visitor.I know that being an astronaut is one of the most difficult and dangerous professions in the world. You have to be brave, determined, highly intelligent, and physically fit. But that's my ultimate dream job - to leave Earth and travel amongst the starsand planets. Our astronaut visitor has made that dream a reality, and I'll get to hear all about it straight from their mouth! I can't wait to shake their hand, have them sign my books, and learn everything I can from someone who has experienced the incredible frontier of space. It's going to be out of this world!篇5Questions I'd Ask an AstronautIf I ever got the chance to talk to a real astronaut, there are so many questions I would want to ask them! Being an astronaut and going to space seems like the coolest job in the entire universe. I can't even imagine what it would be like to leave Earth and float around in zero gravity. I bet astronauts have some amazing stories to tell. Here are some of the top questions I would love to ask an astronaut:What does it feel like when the rocket takes off?I've seen videos of rocket launches, and it looks totally intense with all the fire and smoke blasting out. Does it feel as powerful as it looks when you're strapped in ready for liftoff? Is it scary or exciting or both? I remember going on a roller coaster once and getting that feeling of butterflies in my stomach on the first big drop. I can only imagine that feeling gets multiplied by amillion on a rocket launch! Do your insides feel like they're getting scrambled up?What is your favorite thing about being in space?There are so many parts of being in space that seem amazing to me. Is it the incredible views of Earth from the windows? The experience of floating around in microgravity and not feeling your own weight? Setting off on spacewalks and being outside the spaceship with only your suit between you and the vacuum? Maybe it's just the pride and excitement of few people getting to go to space? I want to know what the astronaut's favorite part is.Do you ever get homesick or miss things from Earth?As great as being in space seems, I imagine it would also be really hard in a lot of ways. You're in a tiny space for months, eating dried food, working long hours, and not getting to see your family or pet your dog. Don't astronauts ever just want a break from the routine to go walk in the park, eat a pizza, and sleep in their own bed? What kinds of things from normal Earth life do they miss the most?Have you ever gotten space sickness? What's that like?I read that a lot of astronauts feel sick and throw up when they first get to space because their inner ear gets confused by the lack of gravity cues. That sounds like it would be the worst! Is space sickness kind of like having a really bad stomach flu where you can't keep anything down? Do you eventually get used to it after being up there for a while? I'd hate to be in a confined space feeling sick with nowhere to go!How do you go to the bathroom in space?This one might be a little gross, but I really want to know! Without gravity, how does, you know...everything not just float away? Do you have to use special zero-gravity space toilets? What if you get sick and have a bathroom emergency in the middle of an hours-long spacewalk? Sorry if these questions are maybe too personal, but inquiring young minds have got to know!What's the food like up there?From what I've seen, it doesn't look that appetizing to eat squeeze tubes of applesauce and bite vacuum-sealed pouches. But I guess food has to be packaged in a way that it won't make a mess in zero-g. Is it all just tasteless mush and freeze-dried ice cream? Or do you get any good meals up there? Do you have afavorite space snack or meal? Being stuck with only yucky food for months would definitely be one of the downsides for me.What's your scariest experience or closest call in space?Being an astronaut seems like such an adventure, but also extremely dangerous when you think about all the things that could potentially go wrong millions of miles from Earth. Have they ever had any terrifying malfunctions or close calls with danger? Did emergency training kick in to save the day? I'm sure astronauts have some incredible stories of times when things went wrong but their skills and keeping a cool head got them through it. I want to hear those heart-pounding tales!Is outer space as cool and fun as it seems?At the end of the day, this is the biggest question I have. Being an astronaut and working in space just seems like the most awesome thing a person could ever do. But maybe there are some not-so-exciting parts that make it more like a regular job too. I want to know if living and working in space is asmind-blowingly amazing as I'm picturing it. Or if the realities of the day-to-day work take some of the novelty away after a while.I just hope I'll get to find out for myself someday if I work really hard and make my dreams come true!So those are the main things I would ask if I was face-to-face with an astronaut. Of course, I'm sure I'd have about a million other questions pop into my head once I was there too. It would be like getting to interrogate a real-life superhero or action movie character about their incredible job. An astronaut's stories and experiences have got to be endlessly fascinating. If I ever get the chance, you can be sure I'm going to fill them with so many questions they'll be begging for a break from this curious kid!篇6A Conversation with an AstronautHave you ever looked up at the night sky and wondered what it would be like to travel to space? I certainly have! Getting the chance to talk to a real astronaut would be a dream come true. If I ever got that amazing opportunity, there are so many questions I would love to ask them about their incredible experiences.First off, I would want to know all about what it feels like to actually blast off into space aboard a rocket ship. Does it make your stomach feel funny from the g-forces? Is it scary or exhilarating? I've seen videos of rocket launches, but I can onlyimagine how loud and powerful it must seem in person as those huge engines ignite. I bet the shaking and vibrations are crazy!Once they made it up into orbit, I'd ask them to describe in detail what the Earth looks like from up in space. We've all seen beautiful photos, but it's got to be breathtaking to actually witness it with your own eyes. Does the planet really look relatively small against the vastness of space? Can you make out continents, clouds, and geographic features? I've heard astronauts say the view is life-changing.Speaking of being in orbit, I'd be super curious to know what it feels like to be in a constant state of freefall and weightlessness. The astronaut could demonstrate some fun zero-gravity tricks like letting a ball of floating water hang in the air. I'd ask if it's hard to eat, sleep, and do normal daily activities when you're weightless. Do they ever get nauseated or seasick from the sensation? It seems like it would take some getting used to!If the astronaut had done a spacewalk before, I'd have a million questions about that too. What does it feel like to step outside into the vacuum of space? Is it scary being attached to the spacecraft by just a tether? Looking down and seeing the entire planet below you must be both amazing and terrifying at the same time. I can't even comprehend how cold it must be outthere too - well below freezing! The astronaut could show me what their bulky spacesuit looks like and describe having to rely on it to stay alive.I'd definitely ask the astronaut if they've ever seen any bizarre sights or had any unusual experiences while in space that even they can't explain. You always hear rumors of astronauts reporting unknown objects or strange phenomena. I'd try to get them to spill the beans on any weird stories! Even if nothing too crazy happened, I bet they still have some interesting tales of equipment failures, close calls, or otherworldly sights.For an astronaut who has been to the Moon, I'd ask them to share what that was like in great detail. Hearing firsthand what it's like to actually walk on the lunar surface would be simply amazing. Did they get to look back at the Earth in the sky? How tough was it to maneuver around in their bulky spacesuit on such low gravity? What did they think when they first stepped foot on an entirely different world? I'd love to hear any other cool stories or fun facts about their moonwalk.No conversation would be complete without asking the astronaut about the intense training process they had to go through just to have the opportunity to go to space. I'd ask them to describe some of the craziest simulations or tests theyendured to prepare their bodies and minds. Things like extreme hot and cold scenarios, survival training, living in simulated space habitats, and all the classroom learning they had to undergo first. It must have taken an incredible amount of hard work and dedication!Finally, I'd make sure to ask the astronaut plenty of questions about what first got them interested in space exploration and what inspired their journey to becoming an astronaut. Was it something they dreamed about sincebeing a little kid? Who were their heroes or role models growing up? What advice would they give to young students today who hope to one day work for NASA or go to space themselves? Getting encouragement and wisdom straight from an astronaut would be incredibly motivating.Can you imagine how cool it would be to shake the hand of someone who has traveled to space and experienced the wonders of the cosmos firsthand? An astronaut would have seen and done things that few humans ever will. I'll never forget getting that once-in-a-lifetime chance to ask them anything I wanted about their incredible journey. It would be a day I'd cherish forever!。

英语作文参观故宫

英语作文参观故宫

02
Besides, when we climbed onto the top of the Tower of Buddhist Incense, a wonderful view came into our sight. What’s more, we walked on the 17-Aech Bridge and visited the stone Archway and we took many fantastic pictures.
In a word, the splendid scenery with so many places of interest makes this trip unforgettable. (It was like a sweet dream. Whenever I think of it, a smile will appear on my face.)
202X
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• 假如你是李华,上周末你和你的家人参观了北 京颐和园绍你的旅游经历。
• 1. 出发时间: 上周六早上七点
准备 • 2.准备物品: 零食,衣服,照相机,雨伞等
• 3.交通方式:乘公交
参观 内容
• 4.主要活动:游览昆明湖,佛香阁,17孔桥和 石坊等景点,并拍照
• As far as I am concerned, the most interesting thing about the trip/ what made me excited is that we took a tour around the Kuming Lake on a beautiful dragon boat. Bathing in the sunshine, I felt extremely comfortable.

外研版新教材Book1 Unit1 Understanding ideas

外研版新教材Book1 Unit1 Understanding ideas

Intensive reading: Find some detailed information.
During the English class
Meng Hao was nervous about introducing himself in front of the class. With 5.___b_u_tt_e_r_f_li_e_s_in__h_i_s_s_to_m__a_c_h__, he began, but everyone laughed. It turned out that he and his teacher shared 6._t_h_e_s_a_m__e_n_a_m__e___.
Intensive reading: Find some detailed information.
After the English class Meng Hao thought he 10.______h_a_d__a__g_o_o_d_b_e_g_i_n_n_in__g to his new school life.
your first day of senior high
Ⅰ Pre-reading
How did you feel on your first day at senior high?
or
excited
nervous
or
proud
curious
What do you like most about your new school? campus
I came to the 3. _c_a_m_p__u_s_ so early that it was still quiet then. It gave me time to 4. _e_x_p_lo_r_e__ it. I had never thought that the first person I met would be my English teacher, Mr Meng! I had my first class with him. Before we started, he asked us to introduce ourselves 5. o_n__e_b_y__o_n_e_. It made me feel like getting 6. b_u_t_t_e_r_fl_ie_sin my stomach. I 7. _b_r_e_a_t_h_e_d deeply and I was so nervous that I found I could only think about my name and my 8. i_n_s_e_ct__co_l_l_ec_t_i_o_n.

Physics Letters B

Physics Letters B

DESY02-096ISSN0418-9833 July2002Search for Excited Electrons at HERAH1CollaborationAbstractA search for excited electron(e∗)production is described in which the electroweak decayse∗→eγ,e∗→eZ and e∗→νW are considered.The data used correspond to anintegrated luminosity of120pb−1taken in e±p collisions from1994to2000with the H1detector at HERA at centre-of-mass energies of300and318GeV.No evidence for a signalis found.Mass dependent exclusion limits are derived for the ratio of the couplings to thecompositeness scale,f/Λ.These limits extend the excluded region to higher masses thanhas been possible in previous direct searches for excited electrons.To be submitted toPhysics Letters BC.Adloff33,V.Andreev24,B.Andrieu27,T.Anthonis4,A.Astvatsatourov35,A.Babaev23,J.B¨a hr35,P.Baranov24,E.Barrelet28,W.Bartel10,S.Baumgartner36,J.Becker37,M.Beckingham21,A.Beglarian34,O.Behnke13,A.Belousov24,Ch.Berger1,T.Berndt14,ot26,J.B¨o hme10,V.Boudry27,W.Braunschweig1,V.Brisson26,H.-B.Br¨o ker2,D.P.Brown10,D.Bruncko16,F.W.B¨u sser11,A.Bunyatyan12,34,A.Burrage18,G.Buschhorn25, L.Bystritskaya23,A.J.Campbell10,S.Caron1,F.Cassol-Brunner22,D.Clarke5,C.Collard4, J.G.Contreras7,41,Y.R.Coppens3,J.A.Coughlan5,M.-C.Cousinou22,B.E.Cox21,G.Cozzika9,J.Cvach29,J.B.Dainton18,W.D.Dau15,K.Daum33,39,M.Davidsson20,B.Delcourt26,N.Delerue22,R.Demirchyan34,A.De Roeck10,43,E.A.De Wolf4,C.Diaconu22,J.Dingfelder13,P.Dixon19,V.Dodonov12,J.D.Dowell3,A.Droutskoi23,A.Dubak25,C.Duprel2,G.Eckerlin10,D.Eckstein35,V.Efremenko23,S.Egli32,R.Eichler32, F.Eisele13,E.Eisenhandler19,M.Ellerbrock13,E.Elsen10,M.Erdmann10,40,e,W.Erdmann36, P.J.W.Faulkner3,L.Favart4,A.Fedotov23,R.Felst10,J.Ferencei10,S.Ferron27,M.Fleischer10,P.Fleischmann10,Y.H.Fleming3,G.Fl¨u gge2,A.Fomenko24,I.Foresti37,J.Form´a nek30,G.Franke10,G.Frising1,E.Gabathuler18,K.Gabathuler32,J.Garvey3,J.Gassner32,J.Gayler10,R.Gerhards10,C.Gerlich13,S.Ghazaryan4,34,L.Goerlich6,N.Gogitidze24,C.Grab36,V.Grabski34,H.Gr¨a ssler2,T.Greenshaw18,G.Grindhammer25, T.Hadig13,D.Haidt10,L.Hajduk6,J.Haller13,B.Heinemann18,G.Heinzelmann11,R.C.W.Henderson17,S.Hengstmann37,H.Henschel35,R.Heremans4,G.Herrera7,44,I.Herynek29,M.Hildebrandt37,M.Hilgers36,K.H.Hiller35,J.Hladk´y29,P.H¨o ting2,D.Hoffmann22,R.Horisberger32,A.Hovhannisyan34,S.Hurling10,M.Ibbotson21,C¸.˙Is¸sever7, M.Jacquet26,M.Jaffre26,L.Janauschek25,X.Janssen4,V.Jemanov11,L.J¨o nsson20,C.Johnson3,D.P.Johnson4,M.A.S.Jones18,H.Jung20,10,D.Kant19,M.Kapichine8,M.Karlsson20,O.Karschnick11,J.Katzy10,F.Keil14,N.Keller37,J.Kennedy18,I.R.Kenyon3, C.Kiesling25,P.Kjellberg20,M.Klein35,C.Kleinwort10,T.Kluge1,G.Knies10,B.Koblitz25, S.D.Kolya21,V.Korbel10,P.Kostka35,S.K.Kotelnikov24,R.Koutouev12,A.Koutov8,J.Kroseberg37,K.Kr¨u ger10,T.Kuhr11,mb3,ndon19,nge35,ˇs toviˇc ka35,30,ycock18,E.Lebailly26,A.Lebedev24,B.Leißner1,R.Lemrani10,V.Lendermann10,S.Levonian10,B.List36,E.Lobodzinska10,6,B.Lobodzinski6,10,A.Loginov23,N.Loktionova24,V.Lubimov23,S.L¨u ders37,D.L¨u ke7,10,L.Lytkin12,N.Malden21,E.Malinovski24,S.Mangano36,R.Maraˇc ek25,P.Marage4,J.Marks13,R.Marshall21,H.-U.Martyn1,J.Martyniak6,S.J.Maxfield18,D.Meer36,A.Mehta18,K.Meier14,A.B.Meyer11,H.Meyer33,J.Meyer10,S.Michine24,S.Mikocki6,stead18, S.Mohrdieck11,M.N.Mondragon7,F.Moreau27,A.Morozov8,J.V.Morris5,K.M¨u ller37, P.Mur´ın16,42,V.Nagovizin23,B.Naroska11,J.Naumann7,Th.Naumann35,P.R.Newman3, F.Niebergall11,C.Niebuhr10,O.Nix14,G.Nowak6,M.Nozicka30,B.Olivier10,J.E.Olsson10, D.Ozerov23,V.Panassik8,C.Pascaud26,G.D.Patel18,M.Peez22,E.Perez9,A.Petrukhin35, J.P.Phillips18,D.Pitzl10,R.P¨o schl26,I.Potachnikova12,B.Povh12,J.Rauschenberger11,P.Reimer29,B.Reisert25,C.Risler25,E.Rizvi3,P.Robmann37,R.Roosen4,A.Rostovtsev23, S.Rusakov24,K.Rybicki6,D.P.C.Sankey5,S.Sch¨a tzel13,J.Scheins10,F.-P.Schilling10,P.Schleper10,D.Schmidt33,D.Schmidt10,S.Schmidt25,S.Schmitt10,M.Schneider22,L.Schoeffel9,A.Sch¨o ning36,T.Sch¨o rner25,V.Schr¨o der10,H.-C.Schultz-Coulon7,C.Schwanenberger10,K.Sedl´a k29,F.Sefkow37,V.Shekelyan25,I.Sheviakov24,1L.N.Shtarkov24,Y.Sirois27,T.Sloan17,P.Smirnov24,Y.Soloviev24,D.South21,V.Spaskov8, A.Specka27,H.Spitzer11,R.Stamen7,B.Stella31,J.Stiewe14,I.Strauch10,U.Straumann37, S.Tchetchelnitski23,G.Thompson19,P.D.Thompson3,F.Tomasz14,D.Traynor19,P.Tru¨o l37, G.Tsipolitis10,38,I.Tsurin35,J.Turnau6,J.E.Turney19,E.Tzamariudaki25,A.Uraev23,M.Urban37,ik24,S.Valk´a r30,A.Valk´a rov´a30,C.Vall´e e22,P.Van Mechelen4,A.Vargas Trevino7,S.Vassiliev8,Y.Vazdik24,C.Veelken18,A.Vest1,A.Vichnevski8,K.Wacker7,J.Wagner10,R.Wallny37,B.Waugh21,G.Weber11,D.Wegener7,C.Werner13,N.Werner37, M.Wessels1,G.White17,S.Wiesand33,T.Wilksen10,M.Winde35,G.-G.Winter10,Ch.Wissing7,M.Wobisch10,E.-E.Woehrling3,E.W¨u nsch10,A.C.Wyatt21,J.ˇZ´aˇc ek30,J.Z´a leˇs´a k30,Z.Zhang26,A.Zhokin23,F.Zomer26,and M.zur Nedden251I.Physikalisches Institut der RWTH,Aachen,Germany a2III.Physikalisches Institut der RWTH,Aachen,Germany a3School of Physics and Space Research,University of Birmingham,Birmingham,UK b4Inter-University Institute for High Energies ULB-VUB,Brussels;Universiteit Antwerpen (UIA),Antwerpen;Belgium c5Rutherford Appleton Laboratory,Chilton,Didcot,UK b6Institute for Nuclear Physics,Cracow,Poland d7Institut f¨u r Physik,Universit¨a t Dortmund,Dortmund,Germany a8Joint Institute for Nuclear Research,Dubna,Russia9CEA,DSM/DAPNIA,CE-Saclay,Gif-sur-Yvette,France10DESY,Hamburg,Germany11Institut f¨u r Experimentalphysik,Universit¨a t Hamburg,Hamburg,Germany a12Max-Planck-Institut f¨u r Kernphysik,Heidelberg,Germany13Physikalisches Institut,Universit¨a t Heidelberg,Heidelberg,Germany a14Kirchhoff-Institut f¨u r Physik,Universit¨a t Heidelberg,Heidelberg,Germany a15Institut f¨u r experimentelle und Angewandte Physik,Universit¨a t Kiel,Kiel,Germany16Institute of Experimental Physics,Slovak Academy of Sciences,Koˇs ice,Slovak Republic e,f 17School of Physics and Chemistry,University of Lancaster,Lancaster,UK b18Department of Physics,University of Liverpool,Liverpool,UK b19Queen Mary and Westfield College,London,UK b20Physics Department,University of Lund,Lund,Sweden g21Physics Department,University of Manchester,Manchester,UK b22CPPM,CNRS/IN2P3-Univ Mediterranee,Marseille-France23Institute for Theoretical and Experimental Physics,Moscow,Russia l24Lebedev Physical Institute,Moscow,Russia e25Max-Planck-Institut f¨u r Physik,M¨u nchen,Germany26LAL,Universit´e de Paris-Sud,IN2P3-CNRS,Orsay,France27LPNHE,Ecole Polytechnique,IN2P3-CNRS,Palaiseau,France28LPNHE,Universit´e s Paris VI and VII,IN2P3-CNRS,Paris,France29Institute of Physics,Academy of Sciences of the Czech Republic,Praha,Czech Republic e,i 30Faculty of Mathematics and Physics,Charles University,Praha,Czech Republic e,i31Dipartimento di Fisica Universit`a di Roma Tre and INFN Roma3,Roma,Italy232Paul Scherrer Institut,Villigen,Switzerland33Fachbereich Physik,Bergische Universit¨a t Gesamthochschule Wuppertal,Wuppertal, Germany34Yerevan Physics Institute,Yerevan,Armenia35DESY,Zeuthen,Germany36Institut f¨u r Teilchenphysik,ETH,Z¨u rich,Switzerland j37Physik-Institut der Universit¨a t Z¨u rich,Z¨u rich,Switzerland j38Also at Physics Department,National Technical University,Zografou Campus,GR-15773 Athens,Greece39Also at Rechenzentrum,Bergische Universit¨a t Gesamthochschule Wuppertal,Germany40Also at Institut f¨u r Experimentelle Kernphysik,Universit¨a t Karlsruhe,Karlsruhe,Germany 41Also at Dept.Fis.Ap.CINVESTAV,M´e rida,Yucat´a n,M´e xico k42Also at University of P.J.ˇSaf´a rik,Koˇs ice,Slovak Republic43Also at CERN,Geneva,Switzerland44Also at Dept.Fis.CINVESTAV,M´e xico City,M´e xico ka Supported by the Bundesministerium f¨u r Bildung und Forschung,FRG,under contract numbers05H11GUA/1,05H11PAA/1,05H11PAB/9,05H11PEA/6,05H11VHA/7and 05H11VHB/5b Supported by the UK Particle Physics and Astronomy Research Council,and formerly by the UK Science and Engineering Research Councilc Supported by FNRS-FWO-Vlaanderen,IISN-IIKW and IWTd Partially Supported by the Polish State Committee for Scientific Research,grant no.2P0310318and SPUB/DESY/P03/DZ-1/99and by the German Bundesministerium f¨u r Bildung und Forschunge Supported by the Deutsche Forschungsgemeinschaftf Supported by VEGA SR grant no.2/1169/2001g Supported by the Swedish Natural Science Research Councili Supported by the Ministry of Education of the Czech Republic under the projectsINGO-LA116/2000and LN00A006,by GAUK grant no173/2000j Supported by the Swiss National Science Foundationk Supported by CONACyTl Partially Supported by Russian Foundation for Basic Research,grant no.00-15-965843Among the unexplained features of the Standard Model(SM)of particle physics is the exis-tence of three distinct generations of fermions and the hierarchy of their masses.One possible explanation for this is fermion substructure,with the constituents of the known fermions being strongly bound together by a new,as yet undiscovered force[1,2].A natural consequence of these models would be the existence of excited states of the known leptons and quarks.Assum-ing a compositeness scale in the TeV region,one would naively expect that the excited fermions have masses in the same energy region.However,the dynamics of the constituent level are un-known,so the lowest excited states could have masses of the order of only a few hundred GeV. Electron1-proton interactions at very high energies provide an excellent environment in which to search for excited fermions of thefirst generation.These excited electrons(e∗)could be singly produced through t-channelγand Z boson exchange.Their production cross-section and par-tial decay widths have been calculated using an effective Lagrangian[3,4]which depends on a compositeness mass scaleΛand on weight factors f and f′describing the relative coupling strengths of the excited lepton to the SU(2)L and U(1)Y gauge bosons,respectively.In this model the excited electron can decay to an electron or a neutrino via the radiation of a gauge boson(γ,W,Z)with branching ratios determined by the e∗mass and the coupling parameters f and f′.In most analyses[5–7]the assumption is made that these coupling parameters are of comparable strength and only the relationships f=+f′or f=−f′are considered.If a relationship between f and f′is assumed,the production cross-section and partial decay widths depend on two parameters only,namely the e∗mass and the ratio f/Λ.In this paper excited electrons are searched for in three samples of data taken by the H1 experiment from1994to2000with a total integrated luminosity of120pb−1.Thefirst sample consists of e+p data accumulated from1994to1997at positron and proton beam energies of27.5GeV and820GeV respectively,and corresponds to an integrated luminosity of37pb−1.A search for excited electrons using this sample of data has been previously published[8].The strategy for the selection of events has been modified from the procedures described in[8]to optimize the sensitivity to higher e∗masses.The two other samples were taken from1998 to2000with an electron or positron beam energy of27.5GeV and a proton beam energy of 920GeV.The integrated luminosities of the e−p and e+p samples are15pb−1and68pb−1, pared to previous H1results[8]the analysis presented here benefits from an increase in luminosity by a factor of more than three and an increase of the centre-of-mass energy from300GeV to318GeV.We search for all electroweak decays e∗→eγ,e∗→eZ and e∗→νW,considering the subsequent Z and W hadronic decay modes only.This leads tofinal states containing an electron and a photon,an electron and jets or jets with missing transverse energy induced by the neutrinos escaping from the detector.The Standard Model backgrounds which could mimic such signatures are neutral current Deep Inelastic Scattering(NC DIS),charged current Deep Inelastic Scattering(CC DIS),QED Compton scattering(or Wide Angle Bremsstrahlung W AB),photoproduction processes(γp)and lepton pair production via the two photon fusion process(γγ).The determination of the contribution of NC DIS processes is performed using two MonteCarlo samples which employ different models of QCD radiation.Thefirst was produced withthe DJANGO[9]event generator which includes QEDfirst order radiative corrections based onHERACLES[10].QCD radiation is implemented using ARIADNE[11]based on the ColourDipole Model[12].This sample,with an integrated luminosity of more than10times the exper-imental luminosity,is chosen to estimate the NC DIS contribution in the e∗→eγanalysis.The second sample was generated with the program RAPGAP[13],in which QEDfirst order radia-tive corrections are implemented as described above.RAPGAP includes the leading order QCDmatrix element and higher order radiative corrections are modelled by leading-log parton show-ers.This sample is used to determine potential NC DIS background in the e∗→νW֒→q¯q and e∗→eZ֒→q¯q searches,as RAPGAP describes better this particular phase space domain[8]. For both samples the parton densities in the proton are taken from the MRST[14]parametriza-tion which includes constraints from DIS measurements at HERA up to squared momentum transfers Q2=5000GeV2[15–18].Hadronisation is performed in the Lund string fragmenta-tion scheme using JETSET[19].The modelling of the CC DIS process is performed using the DJANGO program with MRST structure functions.While inelastic W AB is treated using the DJANGO generator,elastic and quasi-elastic W AB is simulated with the W ABGEN[20]event generator.Direct and resolvedγp processes including prompt photon production are generated with the PYTHIA[21]event generator.Finally theγγprocess is produced using the LPAIR generator[22].For the calculation of the e∗production cross-section and to determine the efficiencies,events have been generated with the COMPOS[23]generator based on the cross-section for-mulae given in reference[3]and the partial decay widths stated in reference[4].Initial stateradiation of a photon from the incoming electron is included.This generator uses the narrowwidth approximation(NW A)for the calculation of the production cross section and takes intoaccount the natural width for the e∗decay.For all values of f/Λrelevant to this analysis thisassumption is valid even at high e∗masses where the natural width of the e∗is of the order ofthe experimental resolution.To give an example,for M e∗=250GeV this resolution is equal to7GeV,10GeV,and12GeV for the eγ,eZ andνW decay modes,respectively.All Monte Carlo samples are subjected to a detailed simulation of the response of the H1detector.The detector components of the H1experiment[24]most relevant for this analysis arebriefly described in the following.Surrounding the interaction region is a system of drift andproportional chambers which covers the polar angle2range7◦<θ<176◦.The tracking sys-tem is surrounded by afinely segmented liquid argon(LAr)calorimeter covering the polar angle√range4◦<θ<154◦[25]with energy resolutions ofσE/E≃12%/E⊕2%for hadrons,obtained in test beam measurements[26,27].The tracking system and calorimeters are surrounded by a superconducting solenoid and an iron yoke instrumented with streamer tubes.Backgrounds not related to e+p or e−p collisions are rejected by requiring that a primary interaction vertex be reconstructed within±35cm of the nominal vertex position,by usingfilters based on the event topology and by requiring an event time which is consistent with the interaction time.Electromagnetic clusters are required to havemore than95%of their energy in the electromagnetic part of the calorimeter and to be isolated from other particles[28].They are further differentiated into electron and photon candidates using the tracking chambers.Jets with a minimum transverse momentum of5GeV are recon-structed from the hadronicfinal state using a cone algorithm adapted from the LUCELL schemein the JETSET package[19].Missing transverse energy(E misst )is reconstructed using the vec-tor sum of energy depositions in the calorimeter cells.The analysis presented in this paper is described extensively in[29].The e∗→eγchannel is characterized by two electromagnetic clusters in thefinal state. The main sources of background are the W AB process,NC DIS with photon radiation or a high energyπ0in a jet and the production of electron pairs viaγγfusion.Candidate events are selected with two electromagnetic clusters in the LAr calorimeter of transverse energy greater than20GeV and15GeV,respectively,and with a polar angle between0.1and2.2radians. The sum of the energies of the two clusters has to be greater than100GeV.If this sum is below 200GeV,the background is further suppressed by rejecting events with a total transverse energy of the two electromagnetic clusters lower than75GeV or with more than two tracks spatially associated to one of the clusters.The numbers of events passing the analysis cuts for the SM background processes and for the data in each of the three samples are given in Table1.About half of the background originates from NC DIS events with most of the remainder being due to W AB events.The efficiency for selecting the signal varies from85%for an e∗mass of150GeV to72%for an e∗mass of250GeV.As in all other channels the efficiencies are derived using samples of1000e∗events generated at different e∗masses.The various sources of systematic error are discussed later.Distributions of the invariant mass of the candidate electron-photon pairs of the three data samples together and for the SM expectation are shown in Fig.1a.Sample e−p920GeVChannel SM background SM background SM background e∗→eγ7.2±1.0±0.1 4.0±0.7±0.215.6±1.7±0.4 e∗→eZ֒→q¯q7.1±2.1±2.8 5.6±0.4±1.225.3±1.9±5.5 e∗→νW֒→q¯q 2.4±0.2±0.7 3.9±0.2±0.7 6.1±0.4±1.5 Table1:Number of candidate events observed in the three decay channels with the correspond-ing SM expectation and the uncertainties on the expectation(statistical and systematic error).The e∗→eZ֒→q¯q channel is characterized by an electromagnetic cluster with an associated track and two high transverse energy jets.The analysis for this channel uses a sample of events with at least two jets with a transverse energy above17GeV and16GeV,respectively,and an electron candidate with a transverse energy E e t>20GeV.These two jets and the electron must have polar angles smaller than2.2radians.Furthermore,to avoid possible double counting of events from the e∗→eγchannel,events with two electromagnetic clusters with transverse energies above10GeV and a total energy of the two clusters greater than100GeV are removed. The main SM contribution is NC DIS as photoproduction events do not yield a significant rate of electron candidates with large E e t.For20GeV<E e t<65GeV,a cut is made on the602468101214161820invariant mass (GeV)e v e n t s0510152025invariant mass (GeV)e v e n t s 012345678910invariant mass (GeV)e v e n t s Figure 1:Invariant mass spectra of candidate (a)eγpairs for the e ∗→eγanalysis,(b)elec-tron and two jets for the e ∗→eZ analysis and (c)neutrino and two jets for the e ∗→νW anal-ysis.Solid points correspond to the data and the histogram to the total expectation from different SM processes.electron polar angle.This ranges from θe <1.35for E e t =20GeV to θe <2.2radians for E e t =65GeV and depends linearly on E e t .The dijet invariant mass has to be in the range −15<M jj −M Z <7GeV .If there are more than two jets,the pair with invariant mass closest to the nominal Z boson mass is chosen as the Z candidate.The two jets chosen are ordered such that E jet 1t >E jet 2t .In many SM events the direction of jet 2is close to the proton direction.To ensure that this jet is well measured,an additional cut on its polar angle,θjet 2>0.2radians,7is applied if its transverse momentum is lower than30GeV.For an electron transverse energy 65GeV<E e t<85GeV two jets with an invariant mass M jj>M Z−30GeV are required. At very high transverse energy,E e t>85GeV,the contribution from NC DIS is very low and no further cuts on M jj are needed.The number of events which remain in the data after these cuts are summarized in Table1and compared with the expected SM contribution(mostly NC DIS events).The efficiency for selecting the signal varies from44%for an e∗mass of150GeV to 62%for an e∗mass of250GeV.Distributions of the invariant mass of the electron and the two jets are shown in Fig.1b for data and for the SM expectation.The e∗→νW֒→q¯q channel is characterized by two jets and missing transverse energy E miss t. The main background originates from CC DIS events with a moderate contribution from photo-production,whereas the NC DIS contribution is suppressed for large E misst .The analysis startsfrom a sample of events with at least two jets with transverse energies above17GeV and16GeV,missing transverse energy E misst >20GeV and no isolated electromagnetic cluster withtransverse energy above10GeV.The jets must have a polar angle below2.2radians.Jets in which the most energetic track enters the boundary region between two calorimeter modules and central jets(θ>0.5radians)are required to contain more than two tracks.This cut re-moves NC DIS events in which the scattered electron is misidentified as a jet.Only events with S=V apevents in a mass interval that varies with the width of the expected signal.At M e ∗=150GeV ,a width of the mass interval of 30GeV is chosen for the e ∗→eγdecay mode and 60GeV is chosen for the decay channels with two jets.Systematic uncertainties are taken into account as in [8].The limits on the product of the e ∗production cross-section and the decay branching ratio are shown in Fig.2.As stated in the introduction,most experiments give f/Λlimits under the assumptions f =+f ′and f =−f ′.The H1limits for each decay channel and after combi-nation of all decay channels are given as a function of the e ∗mass in Fig.3a,for the assumption f =+f ′.With this hypothesis the main contribution comes from the e ∗→eγchannel.The values of the limits for f/Λvary between 5×10−4and 10−2GeV −1for an e ∗mass ranging from 130GeV to 275GeV .These results improve significantly the previously published H1limits for e +p [8]collisions.The LEP experiments [5,6]and the ZEUS collaboration [7]have also reported on excited electron searches.Their limits are shown in Fig.3b.The LEP 2experiments have shown results in two mass domains.In direct searches for excited electrons limits up to a mass of about 200GeV are given.Above 200GeV their results are derived from indirect searches only.The H1limit extends the excluded region to higher masses than reached in previous direct searches.Figure 2:Upper limits at 95%confi-dence level on the product of the pro-duction cross-section σand the decaybranching ratio BR for excited elec-trons e ∗in the various electroweakdecay channels,e ∗→eγ(dashed line),e ∗→eZ ֒→q ¯q (dotted-dashedline)and e ∗→νW ֒→q ¯q (dotted line)as a function of the excited electronmass.The signal efficiencies used tocompute these limits have been deter-mined with events generated under theassumption f =+f ′.1010110e * mass (GeV)σ*B R (p b )More generally,limits on f/Λas a function of f ′/f are shown in Fig.4for three e ∗masses (150,200and 250GeV ).It is worth noting that excited electrons have vanishing electromag-netic coupling for f =−f ′.In this case the e ∗is produced through pure Z boson exchange.As a consequence the production cross-section for excited electrons at HERA is much smaller in the f =−f ′case than in the f =+f ′case.For e ∗masses between 150and 250GeV the ratio910101010e* mass (GeV)f /Λ (G e V -1)10101010e* mass (GeV)f /Λ (G e V -1)Figure 3:Exclusion limits on the coupling f/Λat 95%confidence level as a function of the mass of excited electrons with the assumption f =+f ′.(a)Limit for each decay channele ∗→eγ(dashed line),e ∗→eZ ֒→q ¯q (thick dotted-dashed line),e ∗→νW ֒→q ¯q (dotted line)and for the combination of the three channels (full line).It must be noted that a part of the data included in the present result were used to obtain the previous H1limit [8].(b)Comparison of this analysis with ZEUS results [7](dashed line)and LEP 2results on direct searches [5](dotted-dashed line)and on indirect searches [6](dotted line).of the cross-sections for f =+f ′and f =−f ′varies between 170and 900.For high e ∗masses and some values of the couplings,no limits are given because the natural width of the e ∗would become extremely large.In summary,a search for excited electron production was performed using all the e +p and e −p data accumulated by H1between 1994and 2000.No indication of a signal was found.New limits have been established as a function of the couplings and the excited electron mass for the conventional relationship between the couplings f =+f ′.The dependence of the f/Λlimit on the ratio f ′/f has been shown for the first time at HERA.The data presented here restrict excited electrons to higher mass values than has been possible previously in direct searches.We are grateful to the HERA machine group whose outstanding efforts have made and continue to make this experiment possible.We thank the engineers and technicians for their work in constructing and now maintaining the H1detector,our funding agencies for financial support,the DESY technical staff for continual assistance and the DESY directorate for the hospitality which they extend to the non-DESY members of the collaboration.10Figure 4:Exclusion lim-its on the coupling f/Λat 95%confidence level as a function of the ratio f ′/f for three different masses of the e ∗:150GeV (full line),200GeV (dotted line)and 250GeV (dashed line).10101010f //ff / Λ (G e V -1)References[1]H.Harari,Phys.Rep.104(1984)159.[2]F.Boudjema,A.Djouadi and J.L.Kneur,Z.Phys.C 57(1993)425.[3]K.Hagiwara,D.Zeppenfeld and S.Komamiya,Z.Phys.C 29(1985)115.[4]U.Baur,M.Spira and P.M.Zerwas,Phys.Rev.D 42(1990)815.[5]G.Abbiendi et al.[OPAL Collaboration],CERN-EP/2002-043,arXiv:hep-ex/0206061.Submitted to Phys.Lett.B [6]P.Abreu et al.[DELPHI Collaboration],Eur.Phys.J.C 8(1999)41[hep-ex/9811005].[7]S.Chekanov et al.[ZEUS Collaboration],DESY-01-132arXiv:hep-ex/0109018.[8]C.Adloff et al.,[H1Collaboration],Eur.Phys.J.C 17(2000)567[hep-ex/0007035].[9]G.A.Schuler and H.Spiesberger,in:Proceedings of Physics at HERA ,Hamburg 1991,V ol.3,pp.1419-1432.[10]A.Kwiatkowski,H.Spiesberger and H.J.M¨o hring,mun.69(1992)155.11[11]L.L¨o nnblad,mun.71(1992)15.[12]B.Andersson,G.Gustafson,L.L¨o nnblad and U.Pettersson,Z.Phys.C43(1989)625.[13]H.Jung,mun.86(1995)147.[14]A.D.Martin,R.G.Roberts,W.J.Stirling and R.S.Thorne,Eur.Phys.J.C4(1998)463.[hep-ph/9803445].[15]S.Aid et al.,[H1Collaboration],Nucl.Phys.B470(1996)3[hep-ex/9603004].[16]C.Adloff et al.,[H1Collaboration],Nucl.Phys.B497(1997)3[hep-ex/9703012].[17]M.Derrick et al.,[ZEUS Collaboration],Z.Phys.C69(1996)607[hep-ex/9510009].[18]M.Derrick et al.,[ZEUS Collaboration],Z.Phys.C72(1996)399[hep-ex/9607002].[19]T.Sj¨o strand,hep-ph/9508391,LU-TP-95-20,CERN-TH-7112-93-REV,August1995.[20]C.Berger and P.Kandel,Proceedings of the Workshop Monte Carlo generators for HERAPhysics,Hamburg1998-1999,pp.596-600,[hep-ph/9906541].[21]T.Sj¨o strand,mun.82(1994)74.[22]S.P.Baranov,O.D¨u nger,H.Shooshtari and J.A.Vermaseren,Proceedings of Physics atHERA,Hamburg1991,vol.3,pp.1478-1482.[23]T.K¨o hler,Proceedings of Physics at HERA,Hamburg1991,vol.3,pp.1526-1541.[24]I.Abt et al.,[H1Collaboration],Nucl.Instrum.Meth.A386(1997)310;ibid.348.[25]B.Andrieu et al.,[H1Calorimeter Group],Nucl.Instrum.Meth.A336(1993)460.[26]B.Andrieu et al.,[H1Calorimeter Group],Nucl.Instrum.Meth.A350(1994)57.[27]B.Andrieu et al.[H1Calorimeter Group],Nucl.Instrum.Meth.A336(1993)499.[28]A.Sch¨o ning,Untersuchung von Prozessen mit virtuellen und reellen W±-Bosonen amH1-Detektor bei HERA,Ph.D.Thesis,University of Hamburg,1996.https://www-h1.desy.de/publications/theseslist.html[30]T.Carli,Proceedings of the Workshop Monte Carlo generators for HERA Physics1998-1999,pp.185-194,[hep-ph/9906541].[31]P.Bate,High Transverse Momentum2-jet and3-jet Cross-section Measurements in Pho-toproduction,Ph.D.Thesis,University of Manchester,1999.12。

in search of Davos Man课文翻译

in search of Davos Man课文翻译

In Search of Davos ManIntroductionThe concept of “Davos Man” originated from the World Economic Forum (WEF) held annually in the Swiss ski resort town of Davos. It refers to the global elite - influential individuals who gather at the event to discuss and shape global economic policies. In this article, we will explore the characteristics, impact, and criticisms associated with Davos Man.Characteristics of Davos ManDavos Man is characterized by several distinct features:1.Wealth and Power–Davos Man is typically a member of the global elite,possessing tremendous wealth and wielding immense power invarious domains.–These individuals include corporate leaders, politicians, philanthropists, and influential thinkers. They often shapeeconomic policies that affect nations and societiesworldwide.2.Global Outlook–Davos Man has a strong global orientation, emphasizing the interconnectedness of the world and the need forinternational collaboration.–They advocate for open trade, globalization, and economic integration, believing that these factors drive globalprosperity.3.Technological Savvy–Davos Man recognizes the transformative power of technology and the Fourth Industrial Revolution.–They embrace innovation and digitalization, promotingpolicies that harness technological advancements foreconomic growth and societal development.mitment to Social Causes–Many Davos Man participants are engaged in philanthropy and social endeavors.–Initiatives related to climate change, poverty alleviation, access to healthcare and education, and gender equality areoften discussed and supported by this group.Impact of Davos ManThe influence of Davos Man extends beyond the World Economic Forum. Their impact can be seen in various aspects:1.Economic Policy–Davos Man has significant influence on global economic policies adopted by governments and internationalorganizations.–Their advocacy for free trade, deregulation, andliberalization has shaped the economic landscape of manynations.2.Global Governance–Davos Man plays a crucial role in shaping global governance structures.–They participate in forums like the G7, G20, and United Nations, contributing to discussions on issues such asclimate change, poverty eradication, and sustainabledevelopment.3.Business Practices–Davos Man’s emphasis on corporate social responsibility has driven changes in business practices.–Many corporations now prioritize environmentalsustainability, ethical sourcing, and inclusive workplacepolicies due to the influence of this global elite.4.Social Impact–Davos Man’s involvement in philanthropic effort s hascontributed to social change initiatives worldwide.–Through charitable foundations and collaborations, they have made substantial contributions to education, healthcare, andpoverty reduction.Criticisms of Davos ManDespite their influence, Davos Man is not exempt from criticism. Some common critiques include:1.Elitism–Critics argue that Davos Man represents a disconnected elite who are detached from the realities faced by ordinary people.–They claim that the discussions and decisions made by this group predominantly benefit the wealthy, perpetuating socialand economic inequality.ck of Diversity–The composition of Davos Man often lacks diversity, both in terms of gender and representation from developing nations.–Critics argue that a broader range of perspectives isnecessary to address global challenges effectively.3.Ineffectiveness of Policies–Despite their influence, skeptics question the actual impact of Davos Man’s policies on addressing pressing globalissues.–They argue that a narrow focus on market-driven solutions may not adequately address complex problems like climatechange or income inequality.ck of Accountability–Some argue that Davos Man operates without sufficientaccountability, as decisions made at the Forum are notsubject to democratic processes or public scrutiny.–Critics point out that the concentration of power in the hands of a select few can lead to decisions that prioritizetheir own interests over the common good.ConclusionThe concept of Davos Man represents a global elite that holdssubstantial power and influence over economic policies and global governance. While they have made significant contributions to philanthropy and social causes, criticisms regarding elitism, lack of diversity, policy effectiveness, and accountability persist. Understanding the characteristics and impact of Davos Man is crucial forreflecting on the dynamics of power and shaping a more inclusive and equitable global economy.。

选择性必修第一册 Unit 5 Revealing nature(教师版)

 选择性必修第一册 Unit 5 Revealing nature(教师版)

Ⅰ.阅读单词——会意1.disgrace n.丢脸,耻辱2.beak n.鸟嘴,喙3.giant tortoise巨型陆龟4.comb-like adj.梳状的5.spine n.(动植物的)刺,刺毛6.myth n.(古代的)神话7.pesticide n.杀虫剂,农药8.chilli n.辣椒9.cybercrime n.网络犯罪10.centimetre n.厘米Ⅱ.重点单词——记形1.seed n.种子,籽2.sample n.样本3.ancestor n.(动物的)原种,祖先4.generate v.产生,创造5.characteristic n.特征,特性6.decline v.减少7.blame v.责怪,指责;把……归咎于8.goat n.山羊9.primitive adj.原始的,低等的10.worldwide ad v.遍及全世界11.giant adj.巨大的,特大的12.legend n.传说,传奇(故事) 13.root n.根14.link v.把……联系起来;连接Ⅲ.拓展单词——悉变1.distant adj.遥远的;冷淡的→distance n.距离→distantly ad v.疏远地2.geologist n.地质学家→geology n.地质学3.evolve v.进化→evolution n.进化(论)4.suspect v.猜想,怀疑,觉得→suspicious adj.怀疑的;可疑的5.detect v.发现,察觉(尤指不易觉察到的事物)→detection n.发现→detective n.侦探1.have ...at heart 把……放在心上;热心于做某事2.keep ...on track使……做法对路3.count on信赖;依靠;指望4.indispensable /ˌI nd I'spensəbl/adj.不可缺少的;必需的5.betray /b I'tre I/v t.背叛;出卖;流露6.stick up to支持;捍卫7.take a hit承受打击;遭到破坏;受到严重影响8.nurture /'nɜːtʃə(r)/v t.培育;养育9.undertaking /ˌʌndə'te I k Iŋ/n.任务;事业10.dwell /dwel/v i.居住;栖身dwell on老是想着或唠叨某事(尤指令人不愉快之事)Ⅳ.背核心短语1.answer the call响应号召2.be a disgrace是耻辱,是丢脸的事3.be native to源于……的,原产于……4.first choice 首选5.of all time 有史以来6.in question 正被讨论的,谈论中的7.be crowded with 挤满,充满8.come to exist 开始存在9.adapt to适应10.a variety of 各种各样的11.in the end最后,终于12.be home to...是……的家园13.carry out执行14.tiny amounts of 微量的15.drive...away赶跑;驱车离开16.in some ways在某些方面Ⅴ.悟经典句式1.And that was the answer to how new species of plants and animals came to exist:they evolved from earlier ancestors.(how引导的宾语从句)于是,关于动植物的新种类是如何产生的这个问题就有了答案:它们是从早期的祖先进化而来的。

the search for new,clean阅读理解

the search for new,clean阅读理解

The search for new, clean energy sources has occupied the attention of scient ists and politicians for years. One common resource for green energy is the wind. A new twist on this old resource could cause the energy output of wind -power plants to rocket.Standard wind-power plants rely on solid support and generally can only reac h a height of 200 meters or so. Higher than that, winds tend to be stronger and more consistent, but the challenge is figuring out how to gain the energ y from those winds.Delft University of Technology in the Netherlands and Karlsruhe University of Applied Sciences in Germany have formed a kite-power research group. The g roup is working to develop kites with wings connected to electrical generator s (发电机) on the ground.The research group’s goal is to design a kite that can operate on its own fo r 24 hours. Research has begun, but many challenges remain, including makin g the generators more efficient and perfecting the automatic flight control an d the structure of the kites. Nevertheless in June 2012, they demonstrated th at their kites could operate automatically at an altitude of up to 700 meters. Meanwhile, in Italy, researchers are working on a similar power generator that relies on kites. When the generator, called KiteGen, senses the wind blowing, kites are released from the ends of poles with high-resistance cables (线) to control their height and angle. These cables are able to move the kites if the system senses incoming objects such as planes, helicopters or even individual birds. The kites themselves are light, tough and able to reach fairly high alti tudes. They circle around in the wind, which sets the core of the generator in motion, producing electric current.KiteGen has the potential to be very cost-effective in the long run. After the i nitial cost of designing and setting up the plant, little additional investment will be necessary, apart from standard maintenance. The plant also requires re latively little space, which makes it ideal for cities and means that multiple pl ants can be set up to provide even more energy.Kite power has the potential to greatly improve on current wind-power strate gies. In the future, it may be an efficient, cost-effective supplement (补充) to t he other sources of energy we use, or even a replacement for some of them.1. What does the underlined expression “a new twist” probably mean in the first paragraph?A.A strict standard. B.A challenging task.C.A strong motivation. D.A clever idea.2. If the wind-power plants are higher than 200 meters, what is the problem? A.It is a waste of money. B.It is extremely dangerous.C.It is hard to attain the energy. D.It is totally unrealistic.3. Why do both of the researches adopt kites?A.Kites can fly high. B.Kites are a new trend.C.Kites are eco-friendly. D.Kites can replace old equipment.4. What is the author’s attitude towards kite power?A.Cautious. B.Optimistic. C.Unclear. D.Critical. 答案:DCAB。

China investigates search engine Baidu after student

China investigates search engine Baidu after student

Wei Zexi was diagnosed with a rare form of cancer when he was a sophemore.
Then he searched for some information of treatment and it turns out that a hospital in Beijing has the technology from the USA to cure this cancer. The hospital was listed at the top of his search results.
你认为人性最大的 恶 是什么? he told his miserable experience on ZHIHU which attracts the attention of the public.
The tag #Wei Zexi Advertising Incident# is one of the hottest topics on Sina Weibo, with posts generating 81 million reads.
China investi death search engine in china which is often compared to Google.
He trusted this highly placed search result was what appeared to be the most trusted hospital treatment available to him.
He is a single child and his parent want to spend all the money to save their son.The hospital promise that he will be healthy for he treatment.
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Submitted to the29th International Conference on High-Energy Physics ICHEP98,V ancouver,Canada,July1998SEARCH FOR EXCITED FERMIONS AT HERAH1CollaborationAbstractWe present a search for excited fermions in scattering at HERA using H1data with an integrated luminosity of37pb.All electroweak decays of excited leptons,are considered.The excited quarks are searched for in the and channels.The analysis considers and hadronic decays andfirst generation leptonic decays.No evidence for new particle production is found.Mass dependent exclusion limits on cross sections and coupling constants are derived.Abstract:581Parallel sessions:10Plenary sessions:121IntroductionConvincing evidence for a substructure of fermions could be the discovery of excited quarks and leptons.Electron-proton interactions at very high energies provide an excellent environ-ment to look for excited fermions of thefirst generation.At the collider HERA magnetic-transition couplings of the positron to a gauge boson would allow single production of through channel and boson exchange or single production of through channel boson exchange.In the same way excited quarks could be produced through channel gauge boson exchange between the incoming positron and a quark of the proton.In this paper we report on a search for excited fermions using the data accumulated by the H1experiment at HERA from1994to1997and corresponding to an integrated luminosity of37pb.The positron and proton beam energies were respectively equal to27.5and820 .The excited leptons are studied through all their decays into a lepton and a gauge boson and the excited quark analysis concentrates on the main decays,and.The subsequent gauge bosons(and)decays studied are those involving electrons1,neutrinos or jets.This study corresponds to a statistical increase of more than a factor10compared to previous H1searches[1,2,3].The paper is organized as follows.After a short description of the H1detector and of our preselection in section2,we present briefly in section3the events generators used.Section4 contains the analysis description.The results and their comparison with a similar analysis done by the ZEUS collaboration[4]are reported in parisons with limits obtained on excited leptons by the LEP experiments[5,6,7]and on excited quarks by the Tevatron experiments[8,9]are also shown.Finally,section6summarizes the results.2The H1detectorA full description of the H1detector can be found in reference[10].Here we describe briefly the components which are relevant for this analysis.The interaction region is surrounded by a drift chamber and proportional chamber tracking system covering the angular range(the forward direction,0,from which the polar angle is measured is the proton beam direction).The tracking system is placed into afinely segmented liquid argon calorimeter covering the polar angular range4154.The electromagnetic part is made of lead/argon and the hadronic part of stainless steel/argon[11].For the LAr calorimeter energy resolution of for hadrons have been obtained in test beam measurements[12,13].A lead-scintillatingfiber calorimeter is located in the backward region(154178)of the H1detector[14]2.The tracking system and calorimeters are surrounded by a super-conducting solenoid producing a uniformfield of1.15T in the direction.The analysis uses the data accumulated over periods in which the main H1components, the central jet chambers,the LAr calorimeter,and the luminosity system were fully operational. The preselection of events relies on the requirement of at least one high electromagnetic shower or missing transverse energy.Background not related to collisions is rejected by requiring that the event time coincides with that of the bunch crossing,using topologicalfilters, and by requesting a primary vertex within cm of the nominal vertex value.3GeneratorsThe main Standard Model backgrounds which could mimic the above signatures are neutral cur-rent Deep Inelastic Scattering(NC DIS),charged current Deep Inelastic Scattering(CC DIS), QED Compton scattering and photoproduction processes.Backgrounds from CC DIS and NC DIS are simulated using the event generator DJANGO[16] which includes QEDfirst order radiative corrections and real bremsstrahlung photons based on HERACLES[17].QCD radiation is implemented using ARIADNE[18]and the hadronicfinal state is generated according to the string fragmentation model by JETSET[19].QED compton scattering events are simulated with the event generator EPCOMPT[20]and compared to the predictions of an other QED Compton event generator COMPTON2.0[21](see section 5.1). The inelastic process is taken into account in both generators NC DIS(radiative events)and QED Compton scattering.To avoid a double counting,we used the QED Comp-ton program to generate events with a negative squared four momentum transferred from the incoming proton to thefinal hadronic state below100and the NC DIS one above. The effect of using or not this criterion is taken into account as a systematic error(section 5.1).The MRS H[22]parton distributions in the proton are used for the inelastic scattering. Direct and resolved photoproduction processes,including prompt photon production are simu-lated with the PYTHIA Monte Carlo[23]event generator.Others processes,corresponding to much lower cross sections,such as interactions or production have also been simulated. The process is simulated using the LPAIR generator[24]and the simulation is studied with the EPVEC program[25].The luminosities generated for these Monte Carlos are varying between3times to100times the experimental luminosity.In order to calculate the acceptance of our selection criteria,a Monte Carlo simulation of excited fermion production and decay is necessary.This analysis uses the COMPOS[26]gen-erator which is based on the cross section described in[27]for production and was modified, for generation,following the cross section given in[28].All Monte Carlo generators are interfaced to a full simulation of the H1detector response.4Search for Excited FermionsIn this section we describe the analysis according to the experimental signatures of thefinal states.4.1Final states with no missing transverse momentumWhen only particles in the proton direction remain undetected,longitudinal momentum conser-vation implies that the variable,where and are the energy and the longitu-dinal momentum in a calorimeter cell,has to be equal to2times the energy of the incoming positron.Therefore we apply the cut:(3565)in the following studies unless otherwise stated.This cut rejects photoproduction and CC DIS backgrounds.4.1.1Events with2electromagnetic clusters:the channelThe decay mode is the most distinct channel in which to search for because of its high branching ratio(is expected for masses above150[29])and its very clear signature.The main backgrounds are the QED Compton process with a well separatedpair in thefinal state,NC DIS with photon radiation or an isolated and the two-photon() production of electron pairs,the latter being found to be small.Exclusive analysis:It has been shown[27]that about half of the cross section is expected in the elastic chan-nel.In this case the signature consists of only two electromagnetic clusters and nothing else in the detector.The remaining source of background left is the QED Compton scattering,the NC DIS background being strongly suppressed by the require-ment of no other signals in H1.The selection is described in table1.We require2isolated electromagnetic clusters with a total energy above20(cuts1and2).The require-ment3,where is the invariant mass of the2electromagnetic clusters,reduces the QED Compton background which is at predominantly low electron-photon masses.Re-quirements4and5are loose cuts and use the fact that for)and QED Compton processes the kinematics are ing the polar angles of the2electromag-netic clusters alone,their energies and the invariant mass can be computed and compared to the measured quantities and.Requirement6is the empty detector condition, where is the total energy deposited in the calorimeter.After application of the above cuts319events remain.The expectation from Standard Model processes is(336QED Compton and3).The average efficiency of this selection for masses above50is equal to.12isolated e.m clusters,5and22031042565Table1:Selection requirements for the exclusive analysis.Inclusive analysis:To improve the acceptance,at least for masses above50,we relax the empty detector condition and require events with2high isolated electromagnetic clusters (and and).To reduce the NC DIS contribution with an isolated,a cut on the multiplicity of tracks pointing to the electromagnetic cluster is made.After this selection candidates are selected and the expected Standard Model back-ground is events(QED Compton,NC DIS and).The combined efficiencies of the two selections for are given in table2,as well as those of all other channels described hereafter.The2electromagnetic clusters invariant masses of the candidates are shown infigures1and2for the exclusive and inclusive analyses respectively,together with the expected background for each of the2selections.The shapes of the data distributions and the predictions of the Standard Model are in good agreement.4.1.2Events with more than2electromagnetic clusters:the channel Using the sub-sample of events with2high electromagnetic clusters,a third electromagnetic cluster with5and is requested.An additional cut,to reduce NC DIS background,rejects events having a jet with above15,jets being defined using a cone algorithm of radius in the plane.After this selection3events are left while ()background events are expected(0.7from NC DIS and0.7from).M()50100200658683-464123233743951502501777677915037645614334293535540463935492838434.1.4Events with one photon and a jet:the channelThe production is dominated by exchange with small values of the squared momentum transfer so the scattered positron is often unseen in the detector.Hence the cut on the variable is not used for this channel.Thefinal state is characterized by a photon and a jet.The main backgrounds come from photoproduction processes with prompt production or with highly energetic and NC DIS events when the associated track with the scattered electron is not reconstructed.In this analysis we ask for one high isolated electromagnetic cluster(,)with no track pointing to it within a distance of40 cm.We request a jet with15and and no electron with above5in the LAr calorimeter.35events are selected compared to a background estimation of34.3 5.7events(2.6NC DIS,12.1,and19.6prompt photon).Figure4shows the distributions of the invariant masses for the data and the expected background.No significant excess is seen.4.2Final states with missing transverse momentumIn the analysis of channels involving a neutrino,a minimum missing transverse momentum of20is requested and the variable has to be less than50.To remove events where the missing transverse momentum could come fromfluctuations of the hadronic energy measurement,an additional cut for the channels with jets is made.A variable is defined as the maximum value of the projections of perpendicular to any jet axis.The cut10is applied.4.2.1Events with one photon,missing and a jet:the channelThefinal state contains an isolated electromagnetic cluster with no track pointing to it.As the is produced through-channel boson exchange,most of the times the events contain also the recoil jet.The main background here are the CC DIS events and the NC DIS events with a large missing transverse momentum due tofluctuation of the hadronic shower.The selection criteria are one high isolated electromagnetic cluster(,) and a jet with5.All of the events which survived at this stage are found by visual inspection to be clear cosmic ray induced events,so no candidate is left.The expected Standard Model contribution is equal to1.30.7events(0.7NC DIS and0.6CC DIS).4.2.2Events with one electron,missing and a jet:the channelThe main backgrounds in this channel are the same as in the paragraph4.2.1with in addition production.Cuts select events with one high electron(15and) and a jet(15and).One event survives the selection for an expected background of1.40.3event(0.7NC DIS,0.5,0.2CC DIS).4.2.3Events with2high jets and missing:the andchannelsFor this channel events with2jets having above20,and a di-jet invariant mass above60are selected.Furthermore,to reduce the NC DIS background,events with an electron are rejected.7events are kept,with4of them identified as cosmic rays induced events after visual inspection.The background expectation is equal to3.80.5events with2.8 events from CC DIS,0.8event from photoproduction and0.2event from NC DIS.4.2.4Events with2high electrons and missing:the andchannelsThe selection is based on2high electromagnetic clusters(20and10 with).A cut is applied on the invariant mass in the search for thefirst channel,on the invariant mass for the second one.No candidate has been found,the Standard Model expectation is0.380.16event(0.12,0.16QED Compton,0.1).4.2.5Events with1high electron and missing:the andchannelsThe channel is characterized by only one electron having a large transverse momentum.The non background(cosmics and halo muons)is severe and we increase the minimum missing transverse momentum requirement from20to25.An isolated high electron(20 with)and no jet with above15are requested.This selection accepts12events.However after a visual inspection only one candidate is left.The expected background is equal to3.60.7events(2NC DIS,0.8,0.5CC DIS,0.2QED Compton, 0.1).5Results5.1Upper Limits on Excited Fermion production cross sectionIn the various channels considered in this analysis,the number of observed events are found to be in a good agreement with the predictions of the Standard Model.In addition no evidence is found for any discrepancy between Standard Model expectation for the relevant invariant mass distributions and measurement.Therefore upper limits on the product of the production cross section and the decay chan-nel branching ratio have been derived at the confidence level.These limits are determined as a function of the excited fermion mass.A mass window is displaced over the whole mass range with a step of5.The width of each window is chosen according to the resolution for the corresponding mass.In each mass interval,the number of observed events,the number of expected background events and the signal efficiency are determined and used to extract the upper limit for the signal following the prescription given in the Particle Data Group[30].We take into account statistical and systematic errors in the contributions of the background and the efficiency by folding Gaussian distributions into the integration of the Poisson law used to determine the limit.The errors taken into account on the background determination are the following:The errors due to the limited statistics of the Monte Carlo generations.An error on the absolute electromagnetic energy scale of and on hadronic energy scale of.For the search,two additional errors are taken into account.The QED Compton background expectations given by the2events generators[20,21]are compared and found to be in good agreement.The difference of number of events is less than and is taken into account as a systematic error.The second error comes from the application or not of the value when using together the QED Compton and the NC DIS generators to simulate the inelastic process(see section3).and the errors taken into account on the efficiency determination are:A statistical uncertainty on the signal acceptance which varies between to.For the radiative decays,the model dependence of the excited fermion angular decay distribution is taken into account by comparing the acceptance for isotropic decays to the distribution of the specific model used3.Finally an overall systematic error of on the luminosity is applied.The effect of the systematic errors on the limit is given as percentages in table3.The limit for the decaying in a lepton and a or a is mainly given by thefinal states where theor decays hadronically.The error is dominated by the uncertainty on the absolute calibration of the calorimeters for hadronic clusters,as it is for the for masses below75. Concerning the,the main systematic error comes from the low simulation at low masses(50)and is dominated by the electromagnetic scale uncertainty at higher masses.M()75125200events45156482-171-1110.827-1661-804012593-11Table3:Effect of the systematic errors on the limit on the product of the cross section and the decay channel branching ratio.The values shown are:3For the distribution is where is the angle between the incoming and outgoing fermion in the rest frame.5.2Upper Limits on coupling parametersWe used a specific model[27,28],in which the cross sections depend on coupling constants ,and for the gauge groups,and,and a substructure scale.As-suming relations between and,branching ratios depend only onare given for the and respectively.We assumed,as is conventional,except for the channel which is forbidden unless.For this decay we chose.V alues ofis above values varying betweento for an mass interval of60to185.The same analysis has been done for the where we assumed also and that the has only electroweak couplings(i.e.)(seefigure10).This last assumption is motivated by the results obtained by the Tevatron experiments[8,9].At theabove to.The ZEUS experiment has published results based on their94-95data for an integrated luminosity of9.4pb[4].Their limits,reported onfigures11,12and13,are worse than those extracted from our analysis because we use a larger integrated luminosity.The cross section in collisions is expected to be significantly higher than in collisions.The ZEUS limit extracted from the data[31](integrated luminosity of0.55pb)is also shown on figure12.It is better than the ZEUS limit obtained from data for masses above130 .LEP experiments have also reported searches for excited leptons at center of mass energiesof the order of0.310to10for masses in the80-170range.For the,L3gives the best limits which are of the order of0.3to0.610for masses between80and180. LEP limits are compared to ours onfigures11and12.6SummaryUsing data taken from1994to1997corresponding to an integrated luminosity of37pb,a search for production of excited fermions has been carried out in most of the possible decay channels.No evidence for excited fermions has been found in the channels which are the following,,,,,,,and .New limits for the production of excited fermions in high energy positron proton interactions have been obtained,which improve previous H1results by a factor10.The exclusion domainsof the coupling parameterfor the and are more stringent but limited to excited leptons masses below180,so HERA extends the limits to higher masses.The results obtained on production are complementary to those given by the Tevatron experiments since the is produced via electroweak couplings at HERA and via strong coupling at the collider.References[1]H1collaboration,I.Abt et al,Nucl.Phys.B396,3(1993).[2]H1collaboration,T.Ahmed et al,Phys.Lett.B340,205(1994).[3]H1collaboration,S.Aid et al,Nucl.Phys.B483,44(1997).[4]ZEUS collaboration,J.Breitweg et al,Z.Phys.C76,631(1997).[5]DELPHI collaboration,P.Abreu et al,Phys.Lett.B393,245(1997).L3collaboration,M.Acciarri et al,Phys.Lett.B401,139(1997).[6]OPAL collaboration,K.Ackerstaff et al,Euro.Phys.Journal C1,45(1998).ALEPH collaboration,contribution to the EPS-HEP97conference,Jerusalem(1997).[7]L3collaboration,contribution to ICHEP98,V ancouver,Abstract498.[8]CDF collaboration,F.Abe et al,Phys.Rev.D55,5263(1997).[9]D0collaboration,I.Bertram,FERMILAB-CONF-96/389-E.[10]H1Collaboration,I.Abt et al Nucl.Instrum.Methods A386,310and348(1997).[11]H1Calorimeter Group,B.Andrieu et al,Nucl.Instrum.Methods A336,460(1993).[12]H1Calorimeter Group,B.Andrieu et al,Nucl.Instrum.Methods A344,492(1994).[13]H1Calorimeter Group,B.Andrieu et al,Nucl.Instrum.Methods A350,57(1994)andNucl.Instrum.Methods A336,499(1993).[14]H1SPACAL Group,R.D.Appuhn et al,Nucl.Instrum.Methods A386,397(1997).[15]H1BEMC Group,J.Ban et al,Nucl.Instrum.Methods A372,399(1996).[16]DJANGO6.2:G.A.Schuler and H.Spiesberger,Proc.of the Workshop Physics at HERA,Eds.W.Buchm¨u ller,G.Ingelman,DESY Hamburg1991,V ol3,p1419.[17]HERACLES4.4:A.Kwiatkowski,H.Spiesberger and H.-J.M¨o ring,m.69(1992)155.[18]ARIADNE4.0:L.L¨o nnblad,m.71(1992)15.[19]JETSET7.3and7.4:T.Sj¨o strand,Lund Univ.preprint LU-TP-95-20(August1995)321pp;idem,CERN preprint TH-7112-93(February1994)305pp.[20]EPCOMPT:F.Raupach,Proc.of the Workshop Physics at HERA,Eds.W.Buchm¨u ller,G.Ingelman,DESY Hamburg1991,V ol3,p1473.[21]COMPTON2.0: A.Courau et al.,Proc.of the Workshop Physics at HERA,Eds.W.Buchm¨u ller,G.Ingelman,DESY Hamburg1991,V ol2,p902and V ol3,p1468. [22]A.D.Martin,R.G.Roberts and W.J.Stirling,Proc.of the Workshop on Quantum FieldTheoretical Aspects of High Energy Physics,ed.B.Geyser and E.M.Ilgenfritz,p.11 (1993).[23]PYTHIA5.7:T.Sj¨o strand,CERN-TH-6488(1992),m.82(1994)74.[24]LPAIR:S.P Baranov et al.,Proc.of the Workshop Physics at HERA,Eds.W.Buchm¨u ller,G.Ingelman,DESY Hamburg1991,V ol3,p1478.[25]EPVEC:U.Baur,J.A.M V ermaseren,D.Zeppenfeld,Nucl.Phys.B375,3(1992).[26]T.K¨o hler,Proc.of the Workshop Physics at HERA,Eds.W.Buchm¨u ller,G.Ingelman,DESY Hamburg1991,V ol3,p1526.[27]K.Hagiwara,S.Komamiya and D.Zeppenfeld,Z.Phys.C29,115(1985).[28]G.Jikia,Nucl.Phys.B333,317(1990).[29]U.Baur,M.Spira and P.Zerwas,Phys.Rev.D42,815(1990).[30]R.M.Barnett et al,Phys.Rev.D54,1(1996).[31]ZEUS collaboration,M.Derrick,Z.Phys.C65,627(1995).1011010 2 EM clusters invariant mass (GeV)d N /d M ( /10 Ge Figure 1:Invariant mass of the 2electromagnetic clusters.Squares correspond to the data selected in the exclusive analysis and the histogram to the expected contribution of the QED Compton scattering normalized to the luminosity of the experiment.1011010 2 EM clusters invariant mass (GeV)d N /d M ( /10 Ge Figure 2:Invariant mass of the 2electromagnetic clusters.Squares correspond to the data selected in the inclusive analysis and the histograms to the different expected contributions of Standard Model processes normalized to the luminosity of the experiment.Events with 1 electron and 2 jets101101010electron-jet-jet invariant mass (GeV)d N /d M ( /25 Ge V )Figure 3:Invariant mass of the electromagnetic cluster and the 2jets.Squares correspond to the data and the histogram to the expected contribution of the NC DIS process normalized to the luminosity of the experiment.Events with 1 photon and 1 jet101011010photon-jet Invariant Mass (GeV)d N /d M ( /15 Ge V )Figure 4:Invariant mass of the electromagnetic cluster and the jet.Squares correspond to the data and the histograms to the different expected contributions of Standard Model processes normalized to the luminosity of the experiment.10-210-1110255075100125150175200225250e * Mass (GeV)σ * B R *( p Figure 5:Upper limits at the confidence level on the product of the cross section and the decay channel branching ratio for excited electron production.The full line corresponds to the radiative decay,the dashed and dotted-dashed lines to the and the decays respectively.Decay channels of the gauge boson and are combined.Areas above the curves are excluded.10-210-1110255075100125150175200225250ν*Mass (GeV)σ * B R *( p Figure 6:Upper limits at the confidence level on the product of the cross section and the decay channel branching ratio for excited neutrino production.The full line corresponds to the radiative decay,the dashed and dotted-dashed lines to the and the decays respectively.Decay channels of the gauge boson and are combined.Areas above the curves are excluded.10-210-1110102255075100125150175*********q *Mass (GeV)σ * B R *(p b )Figure 7:Upper limits at the confidence level on the product of the cross section and the decay channel branching ratio for excited quark production in the electromagnetic (full line)and (dashed line)decay channels.Areas above the curves are excluded.10-410-310-210-11255075100125150175200225250e *Mass (GeV)f / Λ (G e V -1)Figure 8:Exclusion limits on coupling constants at the confidence level as a function ofthe mass for excited electron production.The assumptionis made for the different decay channels (full line for radiative,dashed line for and dotted-dashed line for decays).V alues of the couplings above the curves are excluded.10-310-210-11255075100125150175200225250ν*Mass (GeV)f / Λ (G e V -1)Figure 9:Exclusion limits on coupling constants at the confidence level as a function of themass for excited neutrino production.The relationis assumed for the decays involving a or a (dashed line for the and dotted-dashed line for the )and for the radiative decay (full line).V alues of the couplings above the curves are excluded.10-410-310-210-11255075100125150175200225250q * Mass (GeV)f / Λ (G e V -1)Figure 10:Exclusion limits on coupling constants at the confidence level as a function of the mass for excited quark production,assuming and .The radiative decay is shown in full line and the decay in dashed line.V alues of the couplings above the curves are excluded.10-410-310-210-11255075100125150175200225250e * Mass (GeV)f / Λ (G e V -1)Figure 11:Comparison of the limits on the coupling constants at the confidence level from H1,ZEUS and LEP for the .H1and ZEUS [4]limits are represented in full line and dashed line respectively.The dotted line stands for the L3experiment result [7].10-310-210-11255075100125150175*********ν* Mass (GeV)f / Λ (G e V -1)Figure 12:Comparison of the limits on the coupling constants at the confidence level from H1,ZEUS and LEP for the .H1and ZEUS [4,31]limits are represented in full and dashed line respectively.The dotted line stands for the OPAL-ALEPH experiment results [6].10-410-310-210-11255075100125150175*********q * Mass (GeV)f / Λ (G e V -1)Figure 13:Comparison of the limits on the coupling constants at the confidence level from H1and ZEUS for the .H1and ZEUS [4]limits are represented in full and dashed line respectively.。

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