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Proceedings of the Fifth Workshop on Elementary-Particle Picture of the Universe

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KEK-PROC—91-13 JP9206376 PROCEEDINGS OF THE FIFTH WORKSHOP ON ELEMENTARY-PARTICLE PICTURE OF THE UNIVERSE Izu, November 19-21, 1990 NATIONAL LABORATORY FOR HIGH ENERGY PHYSICS, KEK Cover photograph Top Kamiokande Detector Bottom Left INS Air-Core /?-Ray Spectrometer Right BESS (Balloon Experiment with Superconducting Solenoid) Detector Proceedings of the Fifth Workshop on Elementary-Particle Picture of the Universe Izu, November 19-21, 1990 Editors: Masataka Fukugita R.IFP, Kyoto Univ. Atsuto Suzuki KEK KEK Proceedings 91-13 H National Laboratory for High Energy Phy KEK Reports are available from: Technical Information & Library National Laboratory for High Energy Physii 1-1 Oho, Tsukuba-shi Ibaraki-ken, 305 JAPAN Phone: 0298-64-1171 Telex: 3652-534 (Domestic) (0)3652-534 (International) Fax: 0298-64-4604 Cable: KEKOHO Foreword The Fifth Workshop on the Elementary-Particle Picture of the Universe was held at the Izu National Rest House, Minami- Izu, from 19 to 21, November, 1990. The 80 participants included high-energy physicists, nuclear physicists, cosmic-ray physicists and astrophysicists. Both theorists and experimentalists were participated. This was the concluding workshop of a series that started in February, 1987. It was supported by a Grant-in-Aid for "Scientific Research on Priority Areas" by the Ministry of Education "Elementary-Particle Picture of the Universe", after having a few sporadic workshops held over the preceding few years. At that time there was a growing interest in interdisciplinary fields among particle physics and astrophysics: there were large activities searching for proton decay, as a decisive test for grand unification theories, which are closely related to our understanding of the baryon number generation in the universe. 1MB, Kamiokande, Frejus, NUSEX and KGF renewed their results every year. Stimulated by the idea of Mikheyev and Smirnov revived interest was focused on the solar neutrino problem from a particle physics point of view. Interest was even amplified by an announcement made by Davis in the Toyama Symposium (1986) that solar neutrino captures may be correlated with solar activity. Kamiokande-11 was ready for detecting solar neutrinos by the end of 1986. Sliortly after this lime, actually two weeks after our first workshop, we experienced the celebrated supernova SN1987A in the Large Magel­ lanic Cloud. The neutrino signal from that supernova was detected by the Kamiokande-Il and 1MB detectors. It was the first moment in the history of science that theoretically the speculated dynamics of stellcr collapse could be confirmed, with the use of detectors designed for particle physics studies. This neutrino observation triggered a burst of studies in this interdisciplenary field. The ITEP results (1980) for a finite electron neutrino mass, which initiated intensive studies for a "dark matter dominated universe", were still alive. The experimental effort, including a Japanese experiment, was being made to push down a new limit below the window claimed by the ITEP group. Motivated by the successes and failures of a neutrino dark-matter universe, and also by the prediction of an inflationary universe — which itself is also a possible consequence of grand unification — cosmologists were busy try­ ing to understand the large-scale structure of the universe in terms of the hypothetical "cold dark matter" which provides the mass density that makes the universe flat. This "success" promoted a search for cold dark-matter candidates; axions, heavy neutrinos or other -inos. A Japanese sounding rocket which was launched in Feb. 1987, "discovered" a significant distortion in the cosmic microwave background spectrum, which required energetics greater than astrophysicists could account for. A number of speculations were proposed to account for such a distortion. More pure theorists were dedicating their life to the study of super- string theory; many of them optimistically hoped that all of the forces of particle physics could be unified, and even the long-standing particle mass spectrum problem could be solved soon. The Grant-in-Aid project called "Elementary Particle Picture of the Universe started under pressure of these physical backgrounds. The last 5 years since then have provided us with the following results: (1) No evidence has been found for proton decay. The minimal SU(5) model has encountered trouble; (2) The upper limit on the electron neutrino mass has been lowered down to 10 oV. This excludes the finite-mass result of the 1TEP experiment; (;i) The GOBI-/ satellite has undoubtedly disproved the Japanese rocket, discovery. There is no distortion in the cosmic microwave background spectrum; (4) LEP experiments have definitely shown that there are only three generations associated with light neutrinos. This, at the same lime, rules out most of exotic particles with mass < '15 GeV, which would be a candidate for dark matter. Any hypothetical particle henceforth allowed must be weak (SU('2))-charge neutral as well as electric-charge neutral and SU(3)f neutral. Many of the proposed particle models were excluded by this observa­ tion; (5) The "prediction" of inflation (Q0 = 1) is not. supported by the observations. They strongly point towards no < 1; (C) A decline and fall of suporstring studies. The theory was not unique as hoped. The vacuum is not unique either, which requires a non-perturbative study beyond the currently available technique. Suporstring "inspired" phenomenology also turned out to be rather suporstring "independent" phenomenology. Most significant of all, very few people study superstrings any more. These observations clearly consolidated our views, and have forced us to believe that the real world is very close to what the standard theory predicts. Old problems remain intact both in particle physics and astrophysics. Our frustration is that cosmology has not pro­ vided us with any testing grounds for particle theories, nor could particle physics help us to solve any problems in astrophysics so far. There are, however, a few positive aspects which have been clarified during this period: (1) The solar neutrino experiments of Kamiokande-II, when combined with the Homestake result, strongly suggests that the solar neutrino problem originates in neutrino properties that are unexpected from the standard model. The SAGE experiment also supports this view. We should await more confirmative results from SAGE and GALLEX; (2) Precise mass measurements of V and Z lead to an accurate determination of sin20|v, which shows a clear deviation from the value predicted in the original minimal SIF(O) grand unified theory. The value, however, shows remarkable agreement with that pre­ dicted in the minimal SUSY SU(5) model. There are, however, other models ( e.g., SO(10)) which also account for the experiment. In any case this seems to indicate the existence of some new energy scale of the unified theory, which deserves further study. In this workshop most of the time was given to reviews of the present status and prospects of the subjects of the present project as well as some others, in order to find future directions. In the same spirit we held a detector symposium at which we discussed frontier of technology, with the purpose to explore the interdisciplcnary applicability of new technology now being developed. A special session was also arranged for a progress report by representatives of the major experimental groups who received support under the present project. We believe that the workshop was useful to know the status where we are. We hope that the next workshop, when newly held on some other occasions, will bring more success. As organizers we would like to express our gratitude to all of the people who contributed to the workshop; in particular we thank the lecturers and the chairmen as well as younger members of the Kamiokandc group for their assistance in both technical and administrative work. Finally, we would like to acknowledge the support by a Grant-in-Aid for Scientific Research from the Japanese Ministry of Education, Science and Culture. November 1991 M. Fukugita A. Suzuki Workshop Record of "Elementary Particle Picture of the Universe" 1st Workshop: 6-7 February 1987, KEK (Proceedings editted by M.Yoshimura, Y.Totsuka and K.Nakamura) 2nd Workshop: 4-6 February 1988, KEK (Proceedings editted by M.Yoshimura, Y.Totsiika, K.Nakamura and C.S.Lim) 3rd Workshop: 17-19 October 1988, Fujiyoshida (Proceedings cditted by C.S.Lim, M.Mori, A.Suzuki and T.Tanimori) 4th Workshop: 22-25 November 1989, Tateyama (Proceedings editted by K.Hikasa, T.Nakamura T.Ohshima and A.Suzuki) 5th Workshop: 19-21 November 1990, Minami-Izu (Proceedings cditted by M.Fukugita and A.Suzuki) Previous Related Workshop • 13-M February 1979, KEK The Unified Theory and the Baryon Number in the Universe, KEK-79-18 (1979), edit­ ted by O.Sawada and A.Sugamoto • 18-20 October, 1982, Kamioka Monopolcs and Proton Decay, KEK-83-12 (1983), ediUed by J.Arafune and H.Sugawara • 25-27 January, 1983, KEK Grand Unified Theories and Early Universe, KEK-83-13 (1983), editted by M.Fukugita and M.Yoshimura • 7-10 December, 1983, KEK Grand Unified Theories and Cosmology, KEK-84-12 (1984), edittcd by K.Odaka and A.Sugamoto • 15-17 November, 1984, Takayama Towards Unification and its Verification, KEK-S5-4 (1985), editted by Y.Kazama and T.Koikawa • 16-18 April, 1986, Toyama Seventh Workshop on Grand Unification/ICOBAN'SG, World Scientific (1986), editted by J.Arafune Reports on Workshop Related to the Present Project • Proceedings of Workshop on Dark Matter and the Structure of the Universe, Research Institute for Theoretical Physics (RITP), Hiroshima Univ., Takehara 725, Japan, Jan­ uary 29- February 1, 1989, RRK 89-28. • Proceedings of the Summer Workshop on Supcrstrings, KICK, Tsukuba, Japan, August 29- September 3, 1988, KEK Report 88-12. • Proceedings jf the Workshop "Topology, Field Theory and Superstrings", KICK, Tsukuba, Japan, November 6-10, 1989, KEK Report 89-22.
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    Retro Gamer Speed Pretty Quickly, Shifting to a Contents Will Remain the Same

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    Retromagazine 06 Eng.Pdf

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