Proc. Neutrino Astrophysics - MPP Theory Group

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110 in gamma-rays. However, the acceleration of particles to high energies generally requires a low-density plasma. The acceleration of cosmic rays above ∼ 10 18.5 TeV in sources belonging to the Milky Way seems impossible. Among the prime candidates for these ultra-high energy cosmic rays are (radio and gamma-ray emitting) active galactic nuclei [5] and gamma ray bursts [6]. In those sources cooling of accelerated protons (ions dissociate over cosmological distances) is dominated by interactions with low-energy synchrotron photons (from the accelerated electrons). Due to electromagnetic cascading most gamma-rays are shifted to below the TeV range whereas the neutrinos remain unaffected from such reprocessing. Hence the γ/ν-ratio decreases with energy in spite of being a constant function (from decay kinematics) at the production site (if proton-matter collisions dominate the energy loss, the γ/ν-ratio in the TeV range may be constant and of order unity [7]. The total electromagnetic power of the gamma-ray emitting active galactic nuclei can explain the observed extragalactic gamma-ray background and is of the same order as the power in an extragalactic E −2 differential cosmic ray spectrum dominating above 10 6.5 TeV. Therefore, neutrino flux predictions are generally bounded by ∼ 10 −6 GeV cm −2 s −1 st −1 (Fig. 1). The models [8, 9] yield ∼ 300 upward events above TeV per year per km 3 . Figure 1: Overview of theoretical neutrino flux predictions as compiled by R.J. Protheroe during a workshop on high-energy neutrino astrophysics in Aspen, 1996. Labels refer to (a) atmospheric neutrinos (the solid part indicates the part of the spectrum measured by the Frejus experiment), (b) galactic disk in center and anti-center directions (due to Domokos), (c) AGN [11], (d) AGN [8], (e) AGN [9], (f) charm production upper limit [12], (g) GRBs (due to Lee), (h) UHE CRs (due to Stecker), (i) TDs [10] (courtesy of W. Rhode).
A third, more speculative class of high-energy neutrino sources are topological defects producing gauge bosons at the grand-unified-theory scale of ∼ 10 13 TeV [10]. The unstable gauge bosons generate fragmentation jets with ultra-high energy protons, gamma-rays, and neutrinos which may be responsible for the extended air showers with primary energies above the so-called Greisen cutoff at 10 8 TeV above which protons from sources further way than ∼ 30 Mpc lose their energy in interactions with the microwave background. Acknowledgements Many thanks to all the organizers of this very stimulating workshop, in particular to Wolfgang Hillebrandt and Georg Raffelt for inviting me. References [1] T.K. Gaisser, F. Halzen, T. Stanev, Phys. Rep. 258 (1995) 173 [2] M. Catanese, et al. (Whipple collaboration), ApJ 487 (1997) L143 [3] P. Mészáros, M. Rees, ApJ 405 (1993) 278 [4] T.K. Gaisser, R.J. Protheroe, T. Stanev, ApJ 492 (1998) 219 [5] J.P. Rachen, P.L. Biermann, A&A 272 (1993) 161 [6] E. Waxman, ApJ 452 (1995) L1 [7] A. Dar, A. Laor, ApJ 478 (1997) L5 [8] K. Mannheim, Astropart. Phys. 3 (1995) 295 [9] R.J. Protheroe, University of Adelaide Preprint ADP-AT-96-4 (1996) astro-ph/9607165 [10] G. Sigl, D.N. Schrammm, P. Bhattacharjee, Astropart. Phys. 2 (1994) 401 [11] L. Nellen, K. Mannheim, P.L. Biermann, Phys. Rev. D 47 (1993) 5270 [12] W. Rhode, et al., Astropart. Phys. 4 (1996) 21 111
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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
Page 67 and 68: a b Figure 2: Panel a shows the rec
Page 69 and 70: ference). The angular variations of
Page 71 and 72: Figure 1: Neutrino luminosity and e
Page 73 and 74: [9] G.S. Bisnovatyi-Kogan, Astron.
Page 75 and 76: and the mass-to-luminosity ratio of
Page 77 and 78: Figure 1: Time variation of superno
Page 79 and 80: Figure 3: Energy spectra of the sup
Page 81 and 82: Supernova Neutrino Opacities G.G. R
Page 83 and 84: Quasilinear Diffusion of Neutrinos
Page 85 and 86: Assuming a saturated thermal distri
Page 87 and 88: Anisotropic Neutrino Propagation in
Page 89 and 90: So far the damping rate corresponds
Page 91 and 92: Cherenkov Radiation by Massless Neu
Page 93 and 94: on ω so that they are well approxi
Page 95: 2 2 / meff,e m eff 1.0 0.5 0.0 elec
Page 99 and 100: Gamma-Ray Burst Observations D.H. H
Page 101 and 102: Figure 1: The cumulative distributi
Page 103 and 104: [7] Lilly, S., in Critical Dialogue
Page 105 and 106: ) Phase Transitions in Neutron Star
Page 107 and 108: after the collapse began (nb., no e
Page 109 and 110: Models of Coalescing Neutron Stars
Page 111 and 112: Figure 2: Contour plots of the mass
Page 113 and 114: From our torus models we find that
Page 115: High-Energy Neutrinos
Page 120 and 121: 112 Atmospheric Muons and Neutrinos
Page 122 and 123: 114 Today, however, charm productio
Page 124 and 125: 116 Atmospheric Neutrinos in Super-
Page 126 and 127: 118 number of events 300 200 100 (a
Page 128 and 129: 120 Acknowledgements D.K. is suppor
Page 130 and 131: 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
Page 134 and 135: 126 However, in order to operate th
Page 136 and 137: 128 could be gravitationally captur
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
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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
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