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Accretion: A collection of influential papers by A. Treves, L. Maraschi, M. Abramowicz

By A. Treves, L. Maraschi, M. Abramowicz

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Once the neutrino mixing and mass parameters have been measured with some accuracy, a long-baseline experiment should be developed. The KamLAND, Borexino, MiniBooNE, and MINOS experiments are expected to lead—over the next 5 years—to the synthesis necessary for the long-baseline program. A long-baseline target detector is likely to also carry out a proton decay experiment and serve as a supernova neutrino telescope, as well as many other purposes. NEUTRINO PROPERTIES The neutrino has had a very rich history.

1 A comparison of the electromagnetic and neutrino windows on the universe, which is important because both IceCube and a deep underground lab will be sensitive to neutrinos. Astronomers view the universe with light of greatly different wavelengths and energies, from long-wavelength microwaves whose energies are 10,000 times less than that of visible light to very short wavelength gamma rays whose energies are a trillion times greater than that of visible light. By exploiting the full electromagnetic spectrum, astronomers have revealed a great variety of objects in the universe, from the microwave glow of the big bang, to infrared radiation from planets, to the gamma rays emitted by supermassive black holes.

The 32 SCIENCE POTENTIAL OF A DEEP UNDERGROUND LABORATORY cosmic rays create background events that mask the critical events being searched for. It takes 2 miles of rock to absorb the most energetic of the muons created by cosmic-ray protons striking Earth’s atmosphere. At such great depths, the only backgrounds are made by neutrinos (which easily penetrate the whole Earth but, by the same token, interact very seldom) and by local radioactivity in the rock itself. The latter can be shielded by the use of specially purified but otherwise ordinary materials, such as water.

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