Proc. Neutrino Astrophysics - MPP Theory Group

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192 Torsten Soldner Technische Universität München Physik Department E21 D–85747 Garching, Germany email: tsoldner@physik.tu-muenchen.de Michael Stix Kiepenheuer-Institut für Sonnenphysik Freiburg, Germany email: stix@kis.uni-freiburg.de Leo Stodolsky Max-Planck-Institut für Physik Föhringer Ring 6 D–80805 München, Germany email: les@mppmu.mpg.de Rashid Sunyaev Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 D–85740 Garching, Germany email: sunyaev@mpa-garching.mpg.de Jose Valle Department of Physics University of Valencia Valencia, Spain email: valle@flamenco.ific.uv.es Achim Weiss Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 D–85740 Garching, Germany email: weiss@mpa-garching.mpg.de Christopher Wiebusch Institut für Hochenergiephysik DESY-Zeuthen Berlin, Germany email: wiebusch@ifh.de Stan Woosley Lick Observatory University of California at Santa Cruz Santa Cruz CA 95064, USA email: woosley@lick.ucsc.edu email: woosley@ucolick.org Shoichi Yamada Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 D–85740 Garching, Germany email: shoichi@mpa-garching.mpg.de Enrique Zas Max-Planck-Institut für Physik Föhringer Ring 6 D–80805 München, Germany and Universidad de Santiago de Compostela, Spain email: zas@gaes.usc.es
Our Sonderforschungsbereich (SFB) “Astro-Teilchen-Physik” Speaker: Prof. Dr. Franz von Feilitzsch Technische Universität München Physik Department E15 D–85747 Garching, Germany Phone: ++49 +89 289 12511 email: feilitzsch@e15.physik.tu-muenchen.de Deputy Speaker: Prof. Dr. Wolfgang Hillebrandt Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Straße 1 D–85740 Garching, Germany Phone: ++49 +89 3299 3200 email: wfh@mpa-garching.mpg.de Secretary: N.N. Technische Universität München Physik Department E15 D–85747 Garching, Germany Phone: ++49 +89 289 12503 Fax: ++49 +89 289 12680 email: depner@e15.physik.tu-muenchen.de and its Divisions
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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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38 Figure 1: The S(E) factor of 3 H
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40 Solar Neutrinos: Where We Are an
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42 [9] B. Pontecorvo, Chalk River R
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44 Figure 2: The difference between
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Phenomenology of Supernova Explosio
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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
Page 149 and 150: Non-Standard Big Bang Nucleosynthes
Page 151 and 152: ) Non-standard Neutrino Properties
Page 153 and 154: some heating of the plasma. In cont
Page 155 and 156: Big Bang Nucleosynthesis With Small
Page 157 and 158: Neutrinos and Structure Formation i
Page 159 and 160: Photon and Neutrino Backgrounds The
Page 161 and 162: The (photon) temperature at aeq is
Page 163 and 164: spectrum has therefore changed to 1
Page 165 and 166: Figure 4: Growth of structure in CD
Page 167: Future Prospects
Page 170 and 171: 162 Figure 1: Calorimetric β − s
Page 172 and 173: 164 References [1] F. Gatti: Procee
Page 174 and 175: 166 The frequency of Galactic super
Page 176 and 177: 168 Table 1: Comparison of proposed
Page 178 and 179: 170 Neutrinos in Astrophysics José
Page 180 and 181: 172 N eq 7 6.5 6 5.5 5 4.5 4 3.5 3
Page 182 and 183: 174 Figure 4: SN 1987A bounds on FC
Page 184 and 185: 176 [5] A. Joshipura and J. W. F. V
Page 186 and 187: 178 Some Neutrino Events of the 21s
Page 188 and 189: 180 2099: Relic Neutrinos And last
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Page 192 and 193: 184 Tuesday, Oct. 21: Supernova Neu
Page 194 and 195: 186 Michael Altmann Technische Univ
Page 196 and 197: 188 Paolo Gondolo Max-Planck-Instit
Page 198 and 199: 190 Patrizia Meunier Max-Planck-Ins
Page 202 and 203: 194 A Experimental Particle Physics
Page 204: 196 C Astrophysics and Cosmology C1
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Proc. Neutrino Astrophysics - MPP Theory Group

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