Proc. Neutrino Astrophysics - MPP Theory Group

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148 4 He mass fraction fraction fraction 0.40 0.30 0.20 0.10 20% 10% 1% 0% 0% 0% 0.00 0.01 0.10 1.00 10.00 100.00 1000.00 10000.00 Size of antimatter region @ 100 MeV Figure 1: Predicted 4 He mass fraction as a function of the typical antimatter domain size. Length scales are given in proper units at a temperature of T = 100 MeV. The different lines give results for different amounts of antimatter, i.e. the ratio of R = Nantimatter/Nmatter takes values of 0, 1, 10, and 20%, respectively. All models have the same net baryon density. References [1] R.A. Malaney and G.J. Mathews, Phys. Pep. 229 (1993) 145; S. Sarkar, Rept. Prog. Phys. 59 (1996) 1493. [2] K. Jedamzik and G. Fuller, ApJ 423 (1994) 33. [3] F. Balestra, et al., Nuovo Cim. 100A (1988) 323; Yu.A. Batusov et al., Nuovo Cim. Lett. 41 (1984) 223; V.M. Chechetkin, M.Yu. Khlopov, and M.G. Sapozhnikov, Riv. Nuovo Cim. 5 (1982) 1. [4] J.B. Rehm and K. Jedamzik, in preparation. [5] D. Comelli, M. Pietroni, and A. Riotto, Nucl. Phys. B 412 (1994) 441. [6] M. Giovannini and M.E. Shaposhnikov, hep-ph/9710234 (1997); M. Giovannini and M.E. Shaposhnikov, hep-ph/9708303 (1997).
<strong>Neutrino</strong>s and Structure Formation in the Universe Matthias Bartelmann MPI für Astrophysik, P.O. Box 1523, D–85740 Garching, Germany Abstract I review the standard theory of structure formation in the Universe, starting from the assumptions that (i) the Universe is globally described by a Friedmann-Lemaître model, (ii) structure forms via gravitational instability from primordial density fluctuations, and (iii) these primordial density fluctuations were Gaussian in nature. I describe how density fluctuations grow in time, what the density perturbation power spectrum looks like, and why hot dark matter like neutrinos has a considerable impact on the process of structure formation. Introduction The simplest and most widely accepted theory of structure formation in the Universe starts from the following three assumptions: 1. Globally, the Universe is well described by the Friedmann-Lemaître-Robertson-Walker (FLRW) model. 2. Structure formed via gravitational instability from primordial density fluctuations. 3. These primordial density fluctuations were Gaussian in nature. By the first assumption, the global dynamics of the Universe is described in terms of four parameters, viz. the density of ordinary and relativistic matter, the Hubble constant, and the cosmological constant. The second assumption, together with the dynamics implied by the first, specifies how structures grow in time. The third assumption asserts that the statistics of the density fluctuation field is completely specified by its mean and variance. By definition, the mean density contrast is zero, and the variance is specified by the power spectrum, � P(k) = |δ 2 ( � � k)| , (1) where � k is the wave vector of the density perturbation. The power spectrum itself does not depend on the direction of � k because of the (assumed) isotropy of the density fluctuation field. These three basic assumptions provide the structure of this article. I will first describe the global dynamics of FLRW models, then discuss how density fluctuations grow in an expanding universe, and finally describe the gross features of the density fluctuation power spectrum, before I come to the conclusions. Global Dynamics The scale factor a of a FLRW universe is governed by Friedmann’s equation, 149 � �2 ˙a = a 8πG K c2 ρ − 3 a2 , (2)
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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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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
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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: Big Bang Nucleosynthesis With Small
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 202 and 203: 194 A Experimental Particle Physics
Page 204: 196 C Astrophysics and Cosmology C1
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