Proc. Neutrino Astrophysics - MPP Theory Group

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94 Figure 2: The slope of the differential GRB brightness distribution. Non-evolving sources (solid curve) quickly show significant deviation from the Euclidean value −5/2 with increasing redshift. If the GRB rate is proportional to the SFR (see text) the apparent Euclidean slope extends to z ∼ 1 (dashed curve). For greater z the geometry of the universe together with a now decreasing burst rate cause the slope to deviate rapidly from −5/2. of geometry and decreasing SFR then combine and the slope flattens quickly. Comparison with BATSE data suggests that this SFR model deviates from the pseudo-Euclidean slope too abruptly. While several studies [15, 18, 21] report that the observed SFR generates a brightness distribution consistent with BATSE data, our findings support the different result of Petrosian & Lloyd [12], who suggest that other evolutionary effects must be present in addition to the density evolution described by η(z). While a good fit to the data requires a more sophisticated model of source evolution, the basic message is likely to be the same: the logN–logP distribution does not exclude GRB redshifts much greater than unity. Therefore, the absence of the host galaxies predicted by the “minimal” cosmological model does not call the cosmological origin of bursts into question. Instead, host galaxy observations will teach us where bursts occur. References [1] Band, D., and Hartmann, D. H., ApJ 493, in press (1998). [2] Bond, H. E., IAU Circ. 6654 (1997). [3] Connolly, A. J., et al., astro-ph/9706255 (1997). [4] Ellis, R. S., ARAA 35, 389 (1997). [5] Fuller, G. M., and Shi, X., astro-ph/9711020 (1997). [6] Larson, S. B., ApJ 491, in press (1997).
[7] Lilly, S., in Critical Dialogues in Cosmology, ed. N. Turok, Singapore: World Scientific, 1997, p. 465. [8] Madau, P., et al., MNRAS 283, 1388 (1996) [9] Madau, P., et al., astro-ph/9709147 (1997). [10] Metzger, M. R., et al., IAU Circ. 6631, 6655, and 6676 (1997). [11] Paczynski, B., astro-ph/9710086 (1997). [12] Petrosian, V., and Lloyd, N. M., <strong>Proc</strong>. of 4th Symposium on Gamma Ray Bursts, Huntsville 1997, AIP, eds. C. Meegan, R. Preece, and T. Koshut, in press [13] Peebles, P. J. E., Principles of Physical Cosmology, Princeton: Princeton University Press, 1993. [14] Pian, E., et al., ApJ, submitted (1997). [15] Sahu, K. C., et al., ApJ 489, L127 (1997). [16] Schaefer, B. E., in Gamma-Ray Bursts: Observations, Analyses and Theories, eds. C. Ho, R. I. Epstein, and E. E. Fenimore, Cambridge: Cambridge University Press, 1992, p. 107. [17] Schaefer, B. E., et al., ApJ 489, 693 (1997). [18] Totani, T., ApJ486, L71 (1997). [19] Van Paradijs, J., et al., Nature 386, 686 (1997). [20] Vrba, F. J., et al., proceedings of 4th Symposium on Gamma Ray Bursts, Huntsville 1997, AIP, eds. C. Meegan, R. Preece, and T. Koshut, in press [21] Wijers, R.A.M.J., et al., MNRAS, in press (1997). 95
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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
Page 52 and 53: 44 Figure 2: The difference between
Page 55 and 56: Phenomenology of Supernova Explosio
Page 57 and 58: Figure 2: Theoretical classificatio
Page 59 and 60: Supernova Rates Bruno Leibundgut Eu
Page 61 and 62: galaxies, however, and the statisti
Page 63 and 64: Figure 1: The motions of pulsars re
Page 65 and 66: 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: Figure 1: The cumulative distributi
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 118 and 119: 110 in gamma-rays. However, the acc
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
Page 144 and 145: 136
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
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some heating of the plasma. In cont
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Big Bang Nucleosynthesis With Small
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Neutrinos and Structure Formation i
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Photon and Neutrino Backgrounds The
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The (photon) temperature at aeq is
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spectrum has therefore changed to 1
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Figure 4: Growth of structure in CD
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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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