Proc. Neutrino Astrophysics - MPP Theory Group

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176 [5] A. Joshipura and J. W. F. Valle, Nucl. Phys. B397 (1993) 105 and references therein [6] A. Zee, Phys. Lett. B93 (1980) 389; K. S. Babu, Phys. Lett. B203 (1988) 132 [7] Marco A. Díaz, Jorge C. Romão and José W. F. Valle, hep-ph/9706315; M. A. Diaz, A. Joshipura, J. W. F. Valle, in preparation; For additional papers on neutrino masses in broken R–parity models see: F. Vissani and A. Yu. Smirnov, Nucl. Phys. B460, 37-56 (1996). R. Hempfling, Nucl. Phys. B478, 3 (1996), and hep-ph/9702412; H.P. Nilles and N. Polonsky, Nucl. Phys. B484, 33 (1997); B. de Carlos, P.L. White, Phys.Rev. D55 4222-4239 (1997); E. Nardi, Phys. Rev. D55 (1997) 5772; S. Roy and B. Mukhopadhyaya, Phys. Rev. D55, 7020 (1997). [8] E. Kolb, M. Turner, The Early Universe, Addison-Wesley, 1990, and references therein [9] J. Bardeen, J. Bond and G. Efstathiou, Astrophys. J. 321 (1987) 28; J. Bond and G. Efstathiou, Phys. Lett. B265 (1991) 245; M. Davis et al., Nature 356 (1992) 489; S. Dodelson, G. Gyuk and M. Turner, Phys. Rev. Lett. 72 (1994) 3754; H. Kikuchi and E. Ma, Phys. Rev. D51 (1995) 296; H. B. Kim and J. E. Kim, Nucl. Phys. B433 (1995) 421; M. White, G. Gelmini and J. Silk, Phys. Rev. D51 (1995) 2669 A. S. Joshipura and J. W. F. Valle, Nucl. Phys. B440 (1995) 647. [10] J. Schechter, J. W. F. Valle, Phys. Rev. D25 (1982) 774 [11] J. W. F. Valle, Phys. Lett. B131 (1983) 87; G. Gelmini, J. W. F. Valle, Phys. Lett. B142 (1984) 181; J. W. F. Valle, Phys. Lett. B159 (1985) 49; M. C. Gonzalez-Garcia, J. W. F. Valle, Phys. Lett. B216 (1989) 360. A. Joshipura, S. Rindani, Phys. Rev. D46 (1992) 3000; J. C. Romão, J. W. F. Valle, Nucl. Phys. B381 (1992) 87-108 [12] R.F. Carswell, M. Rauch, R.J. Weynman et al., MNRAS 268 (1994) L1; A. Songalia, L.L. Cowie, C. Hogan and M. Rugers, Nature 368 (1994) 599; D. Tytler and X.M. Fan, Bull. Am. Astr. Soc. 26 (1994) 1424; D. Tytler, talk at the Texas Symposium, December 1996. [13] N. Hata et al., Phys. Rev. Lett. 75 (1995) 3977; C.J. Copi, D.N. Schramm and M.S. Turner, Science 267 (1995) 192 and Phys. Rev. Lett. 75 (1995) 3981; K. A. Olive and G. Steigman, Phys. Lett. B354 (1995) 357-362; S. Sarkar, Rep. on Prog. in Phys. 59 (1997) 1493; P. J. Kernan and S. Sarkar, Phys. Rev. D 54 (1996) R3681 [14] E. W. Kolb, M. S. Turner, A. Chakravorty and D. N. Schramm, Phys. Rev. Lett. 67 (1991) 533; A.D. Dolgov and I.Z. Rothstein, Phys. Rev. Lett. 71 (1993) 476. [15] A.D. Dolgov, S. Pastor, and J.W.F. Valle, Phys. Lett. B383 (1996) 193-198; [hepph/9602233]. For related papers see Hannestad and Madsen Phys. Rev. Lett. 77 (1996) 5148, Phys. Rev. D54 (1996) 7894; J. Rehm, G. Raffelt and A. Weiss Astron. Astron. & Astrophys. 327 (1997) 443; B. Fields, K. Kainulainen and K. Olive, Astropart. Phys. 6 (1997) 169 [16] A.D. Dolgov, S. Pastor, J.C. Romão and J.W.F. Valle, Nucl. Phys. B496 (1997) 24-40 [hep-ph/9610507]. [17] A Masiero, J. W. F. Valle, Phys. Lett. B251 (1990) 273; J. C. Romao, C. A. Santos, and J. W. F. Valle, Phys. Lett. B288 (1992) 311
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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
Page 134 and 135: 126 However, in order to operate th
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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
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 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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