Proc. Neutrino Astrophysics - MPP Theory Group

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194 A Experimental Particle Physics A1 Spectroscopy of Solar Neutrinos A1-1 Borexino A1-2 Development of Cryogenic Detectors for GNO Principal Investigator 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 A2 Experiments on the Decay of the Free Neutron Principal Investigator Prof. Dr. Klaus Schreckenbach Technische Universität München Physik Department E21 D–85747 Garching, Germany Phone: ++49 +89 289 12183 email: kschreck@physik.tu-muenchen.de A3 Development and Application of Cryogenic Detectors for Dark Matter Detection via elastic WIMP-nucleus scattering Principal Investigator 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 A4 Weak Decays of Highly Ionized Nuclei Principal Investigator Prof. Dr. Paul Kienle Technische Universität München Physik Department E12 D–85747 Garching, Germany Phone: ++49 +89 289 12421 email: paul.kienle@physik.tu-muenchen.de
B Theoretical Particle Physics and Statistical Methods B1 Extensions of the Standard Model in View of Applications to Astrophysics and Cosmology Principal Investigator Prof. Dr. Manfred Lindner Technische Universität München Physik Department T30 D–85747 Garching, Germany Phone: ++49 +89 289 12196 email: lindner@physik.tu-muenchen.de B2 String Cosmology Principal Investigator Prof. Dr. Stefan Theisen Ludwig-Maximilians-Universität Sektion Physik Theresienstraße 37 D–80333 München, Germany Phone: ++49 +89 2394 4375 email: theisen@mppmu.mpg.de B3 Morphology of Cosmological Structures Principal Investigator Prof. Dr. Herbert Wagner Ludwig-Maximilians-Universität Sektion Physik Theresienstraße 37 D–80333 München, Germany Phone: ++49 +89 2394 4537 email: wagner@stat.physik.uni-muenchen.de B4 Electroweak Symmetry Breaking in View of Astrophysics and Cosmology Principal Investigator Prof. Dr. Manfred Lindner Technische Universität München Physik Department T30 D–85747 Garching, Germany Phone: ++49 +89 289 12196 email: lindner@physik.tu-muenchen.de 195
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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
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Non-Standard Big Bang Nucleosynthes
Page 151 and 152: ) Non-standard Neutrino Properties
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Page 157 and 158: Neutrinos and Structure Formation i
Page 159 and 160: Photon and Neutrino Backgrounds The
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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 200 and 201: 192 Torsten Soldner Technische Univ
Page 204: 196 C Astrophysics and Cosmology C1
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