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arXiv:astro-ph/9801320v1 30 Jan 199
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Preface This was the fourth worksho
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vi S.J. Hardy Quasilinear Diffusion
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viii
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History of Neutrino Physics: Pauli
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Brief an Oskar Klein, Stockholm, vo
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Recent observations with the Hubble
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MACHO sample of ∼100,000 light cu
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Solar Neutrinos
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14 In the depth range where an abun
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16 as follows: (1) All the detector
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18 [3] J.N. Bahcall and H.A. Bethe,
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20 the opacity has a very slowly ch
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22 Status of the Radiochemical Gall
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24 known true source activity. The
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26 Solar Neutrino Observation with
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28 Events/day/kton/bin 0.3 0.25 0.2
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30 log(Δm 2 (eV 2 log(Δm )) 2 (eV
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32 Table 1: Neutrino event rates in
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34 tank and sphere high purity wate
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36 Measurements of Low Energy Nucle
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- Page 50 and 51: 42 [9] B. Pontecorvo, Chalk River R
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- Page 55 and 56: Phenomenology of Supernova Explosio
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- Page 71 and 72: Figure 1: Neutrino luminosity and e
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- Page 83 and 84: Quasilinear Diffusion of Neutrinos
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- Page 89 and 90: So far the damping rate corresponds
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- Page 102 and 103: 94 Figure 2: The slope of the diffe
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- Page 106 and 107: 98 of the engine itself). A longer
- Page 108 and 109: 100 Acknowledgements We thank Alexa
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- Page 119 and 120: A third, more speculative class of
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- Page 123 and 124: [13] A. Dar and N.J. Shaviv, Astrop
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- Page 127 and 128: Data Monte Carlo total νe CC νµ
- Page 129 and 130: Neutrino Astronomy with AMANDA Ch.
- Page 131 and 132: Thus an Amanda optical module consi
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- Page 135 and 136: High Energy Neutrino Astronomy with
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140 subtraction requires considerab
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142 i) Inhomogeneity in the Baryon-
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144 possibility seems to be ruled o
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146 References [1] R.V. Wagoner, W.
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148 4 He mass fraction fraction fra
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150 where I have ignored the cosmol
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152 We can therefore calculate thei
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154 In other words, the fast radiat
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156 Figure 2: The comoving free-str
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158 • Rapid radiation-driven expa
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Neutrino Experiments with Cryogenic
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produced in the target by neutrino
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OMNIS—A Galactic Supernova Observ
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The proposed detector array is refe
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a cosmologically-significant neutri
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to neutrino masses that vanish as t
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g 10 -3 10 -4 10 -5 1 10 m(ν τ )
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Figure 6: Supernovae shock reheatin
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[18] For a recent ref. see S. Hanne
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2030: Neutrino Thermometer Now we
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[7] For this point, as well as a lo
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Monday, Oct. 20: Solar Neutrinos 10
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Thursday, Oct. 23: High Energy Neut
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Arnon Dar Department of Physics and
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Matthias Junker Laboratori Nazional
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Marisa Sarsa Technische Universitä
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Our Sonderforschungsbereich (SFB)
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B Theoretical Particle Physics and