Proc. Neutrino Astrophysics - MPP Theory Group

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174 Figure 4: SN 1987A bounds on FCNC neutrino interactions. Figure 5: Supernovae and FCNC neutrino interactions. R-process. tory. In Fig. 4 we display the SN 1987A constraints on explicit R-parity-violating FCNCs in the presence of non-zero neutrino masses in the hot dark matter eV range. In Fig. 5 we display the sensitivity of the r-process argument to the presence of FCNC neutrino interactions. Taken altogether, Fig. 4 and Fig. 5 disfavour a leptoquark interpretation of the recent HERA anomaly. As a final example of how astrophysics can constrain neutrino properties we consider the case of resonant νe → νs and ¯νe → ¯νs conversions in supernovae, where νs is a sterile neutrino [25], which we assume to be in the hot dark matter mass range. The implications of such a scenario for the supernova shock re-heating, the detected ¯νe signal from SN 1987A and for the r-process nucleosynthesis hypothesis have been recently analysed [25]. In Fig. 6,
Figure 6: Supernovae shock reheating argument and νe − νs neutrino conversions. taken from ref. [25], we illustrate the sensitivity of the supernova shock re-heating argument to active-sterile neutrino mixing and mass difference. Notice that for the case of r-process nucleosynthesis there is an allowed region for which the r-process can be enhanced. Acknowledgements Supported by DGICYT grant PB95-1077 and in part by EEC under the TMR contract ERBFMRX-CT96-0090. It is a pleasure to thank the organizers for a very friendly atmosphere. References [1] For reviews on the status of neutrino mass see A. Yu. Smirnov, Neutrino Masses and Oscillations, Plenary talk given at 28th International Conference on High energy physics, July 1996, Warsaw, Poland, hep-ph 9611465; and Neutrinos Properties Beyond the Standard Model, J. W. F. Valle, Plenary talk, WIN97, Capri, Italy, June 1997, hepph/9709365. [2] M Gell-Mann, P Ramond, R. Slansky, in Supergravity, ed. D. Freedman et al. (1979); T. Yanagida, in KEK lectures, ed. O. Sawada et al. (1979); R.N. Mohapatra and G. Senjanovic, Phys. Rev. D23 (1981) 165 and Phys. Rev. Lett. 44 (1980) 912 and references therein. [3] Y. Chikashige, R. Mohapatra, R. Peccei, Phys. Rev. Lett. 45 (1980) 1926 [4] For reviews see J. W. F. Valle, Gauge Theories and the Physics of Neutrino Mass, Prog. Part. Nucl. Phys. 26 (1991) 91-171 175
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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
Page 132 and 133: 124 (a.u) 0.5 0.4 0.3 0.2 0.1 0 0 1
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Page 138 and 139: 130 Ground-Based Observation of Gam
Page 140 and 141: 132 Figure 2: Sensitivities in unit
Page 142 and 143: 134 Crab flux Figure 4: Gamma-ray f
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Page 147 and 148: 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
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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 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 202 and 203: 194 A Experimental Particle Physics
Page 204: 196 C Astrophysics and Cosmology C1
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