- Page 1 and 2: arXiv:astro-ph/9801320v1 30 Jan 199
- Page 3: Preface This was the fourth worksho
- Page 6 and 7: vi S.J. Hardy Quasilinear Diffusion
- Page 11 and 12: History of Neutrino Physics: Pauli
- Page 13 and 14: Brief an Oskar Klein, Stockholm, vo
- Page 15 and 16: Recent observations with the Hubble
- Page 17 and 18: MACHO sample of ∼100,000 light cu
- Page 19: Solar Neutrinos
- Page 22 and 23: 14 In the depth range where an abun
- Page 24 and 25: 16 as follows: (1) All the detector
- Page 26 and 27: 18 [3] J.N. Bahcall and H.A. Bethe,
- Page 28 and 29: 20 the opacity has a very slowly ch
- Page 30 and 31: 22 Status of the Radiochemical Gall
- Page 32 and 33: 24 known true source activity. The
- Page 34 and 35: 26 Solar Neutrino Observation with
- Page 36 and 37: 28 Events/day/kton/bin 0.3 0.25 0.2
- Page 38 and 39: 30 log(Δm 2 (eV 2 log(Δm )) 2 (eV
- Page 40 and 41: 32 Table 1: Neutrino event rates in
- Page 42 and 43: 34 tank and sphere high purity wate
- Page 44 and 45: 36 Measurements of Low Energy Nucle
- Page 46 and 47: 38 Figure 1: The S(E) factor of 3 H
- Page 48 and 49: 40 Solar Neutrinos: Where We Are an
- Page 50 and 51: 42 [9] B. Pontecorvo, Chalk River R
- Page 52 and 53: 44 Figure 2: The difference between
- Page 55 and 56: Phenomenology of Supernova Explosio
- Page 57 and 58: Figure 2: Theoretical classificatio
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Supernova Rates Bruno Leibundgut Eu
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galaxies, however, and the statisti
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Figure 1: The motions of pulsars re
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Convection in Newly Born Neutron St
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a b Figure 2: Panel a shows the rec
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ference). The angular variations of
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Figure 1: Neutrino luminosity and e
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[9] G.S. Bisnovatyi-Kogan, Astron.
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and the mass-to-luminosity ratio of
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Figure 1: Time variation of superno
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Figure 3: Energy spectra of the sup
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Supernova Neutrino Opacities G.G. R
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Quasilinear Diffusion of Neutrinos
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Assuming a saturated thermal distri
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Anisotropic Neutrino Propagation in
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So far the damping rate corresponds
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Cherenkov Radiation by Massless Neu
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on ω so that they are well approxi
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2 2 / meff,e m eff 1.0 0.5 0.0 elec
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Gamma-Ray Burst Observations D.H. H
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Figure 1: The cumulative distributi
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[7] Lilly, S., in Critical Dialogue
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) Phase Transitions in Neutron Star
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after the collapse began (nb., no e
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Models of Coalescing Neutron Stars
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Figure 2: Contour plots of the mass
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From our torus models we find that
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High-Energy Neutrinos
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110 in gamma-rays. However, the acc
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112 Atmospheric Muons and Neutrinos
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114 Today, however, charm productio
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116 Atmospheric Neutrinos in Super-
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118 number of events 300 200 100 (a
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120 Acknowledgements D.K. is suppor
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122 Key signatures for νµ nucleon
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124 (a.u) 0.5 0.4 0.3 0.2 0.1 0 0 1
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126 However, in order to operate th
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128 could be gravitationally captur
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130 Ground-Based Observation of Gam
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132 Figure 2: Sensitivities in unit
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134 Crab flux Figure 4: Gamma-ray f
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136
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Helium Absorption and Cosmic Reioni
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Non-Standard Big Bang Nucleosynthes
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) Non-standard Neutrino Properties
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some heating of the plasma. In cont
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Big Bang Nucleosynthesis With Small
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Neutrinos and Structure Formation i
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Photon and Neutrino Backgrounds The
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The (photon) temperature at aeq is
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spectrum has therefore changed to 1
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Figure 4: Growth of structure in CD
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Future Prospects
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162 Figure 1: Calorimetric β − s
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164 References [1] F. Gatti: Procee
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166 The frequency of Galactic super
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168 Table 1: Comparison of proposed
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170 Neutrinos in Astrophysics José
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172 N eq 7 6.5 6 5.5 5 4.5 4 3.5 3
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174 Figure 4: SN 1987A bounds on FC
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176 [5] A. Joshipura and J. W. F. V
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178 Some Neutrino Events of the 21s
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180 2099: Relic Neutrinos And last
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182
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184 Tuesday, Oct. 21: Supernova Neu
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186 Michael Altmann Technische Univ
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188 Paolo Gondolo Max-Planck-Instit
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190 Patrizia Meunier Max-Planck-Ins
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192 Torsten Soldner Technische Univ
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194 A Experimental Particle Physics
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196 C Astrophysics and Cosmology C1