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Henry Tsz-King Wong
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This article presents an overview of neutrino physics research, with highlights on the physics goals, results and interpretations of the current neutrino experiments and future directions and program. It is not meant to be a comprehensive account or detailed review article. Interested readers can pursue the details via the listed references.
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This article reviews the research program and efforts for the TEXONO Collaboration on neutrino and astro-particle physics. The ``flagship program is on reactor-based neutrino physics at the Kuo-Sheng (KS) Power Plant in Taiwan. A limit on the neutrino magnetic moment of $munuebar < 1.3 X 10^{-10} mub}$ at 90% confidence level was derived from measurements with a high purity germanium detector. Other physics topics at KS, as well as the various R&D program, are discussed
The symmetry between quarks and leptons suggests that neutrinos should have mass. As embodied in the grand unified theory SO(10) this yields masses that can only be detected by neutrino oscillations. Such oscillations could be very important for supernova physics. Present observations of solar neutrinos when combined with standard solar model calculations imply particular parameters for neutrino masses and mixings. If the solar model is somewhat relaxed quite different possibilities emerge, which yield very different predictions for future experiments.
RHIC-STAR is a mid-rapidity collider experiment for studying high energy nuclear collisions. The main physics goals of STAR experiment are 1) studying the properties of the strongly coupled Quark Gluon Plasma, 2) explore the QCD phase diagram structure. In these proceedings, we will review the recent results of heavy ion physics at STAR.
Its been a remarkable decade in neutrino physics. Ten years ago this summer, at the 1998 neutrino conference in Takayama, the Super-Kamiokande collaboration reported the observation of neutrinos changing flavor, thereby establishing the existence of neutrino mass. A few years later, the SNO experiment solved the long-standing solar neutrino problem demonstrating that it too was due to neutrino oscillation. Just a few years after that, these effects were confirmed and the oscillation parameters were measured with man-made neutrino sources. Now, just in this last year, the same neutrinos which were the source of the 30 year old solar neutrino problem were measured for the first time in a real-time experiment. In this talk, I will explain how a set of experiments, especially ones in the last few years, have established a consistent framework of neutrino physics and also explain some outstanding questions. Finally, I will cover how a set of upcoming experiments hope to address these questions in the coming decade.
Neutrino telescopes can observe neutrino interactions starting at GeV energies by sampling a small fraction of the Cherenkov radiation produced by charged secondary particles. These experiments instrument volumes massive enough to collect substantial samples of neutrinos up to the TeV scale as well as small samples at the PeV scale. This unique ability of neutrino telescopes has been exploited to study the properties of neutrino interactions across energies that cannot be accessed with man-made beams. Here we present the methods and results obtained by IceCube, the most mature neutrino telescope in operation, and offer a glimpse of what the future holds in this field.
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