Proc. Neutrino Astrophysics - MPP Theory Group

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146 References [1] R.V. Wagoner, W.A. Fowler, and F. Hoyle, ApJ 148 (1967) 3; M.S. Smith, L.H. Kawano, and R.A. Malaney, ApJ Suppl. 85 (1993) 219, C.J. Copi, D.N. Schramm, and M.S. Turner, Science 267 (1995) 192. [2] R.A. Malaney and G.J. Mathews, Phys. Pep. 229 (1993) 145; S. Sarkar, Rept. Prog. Phys. 59 (1996) 1493. [3] J.H. Applegate, C.J. Hogan, and R.J. Scherrer, Phys. Rev. D 35 (1987) 1151; G.J. Mathews, B.S. Meyer, C.R. Alcock, and G.M. Fuller, ApJ 358 (1990) 36; K. Jedamzik, G.M. Fuller, and G.J. Mathews, ApJ 423 (1994) 50. [4] K.E. Sale and G.J. Mathews, ApJ 309 L1. [5] K. Jedamzik and G.M. Fuller, ApJ 452 33. [6] C.J. Copi, K.A. Olive, and D.N. Schramm, ApJ 451 (1995) 51. [7] J. Rehm and K. Jedamzik, this volume. [8] F. Balestra, et al., Nuovo Cim. 100A (1988) 323. [9] 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. [10] E.W. Kolb and R.J. Scherrer, Phys. Rev. D 25 (1982) 1481. [11] S. Dodelson, G. Gyuk, and M.S. Turner, Phys. Rev. D 49 (1994) 5068. [12] M. Kawasaki, P. Kernan, H.-S. Kang, R.J. Scherrer, G. Steigman, and T.P. Walker, Nucl. Phys. B 419 (1994) 105. [13] M. Kawasaki, K. Kohri, and K. Sato, astro-ph/9705148. [14] N. Terasawa and K. Sato, Phys. Lett. B 185 (1988) 412. [15] S. Hannestad, hep-ph/9711249. [16] R. Barbieri and A. Dolgov, Phys. Lett. B 237 (1990) 440; K. Enquist, K. Kainulainen, and J. Maalampi, Phys. Lett. B 249 531. [17] R. Foot and R.R. Volkas, hep-ph/9706242. [18] G. Beaudet and A. Yahil, ApJ 218 (1977) 253; K.A. Olive, D.N. Schramm, D. Thomas, and T.P. Walker, Phys. Lett. B 265 (1991) 239. [19] D.A. Dicus, E.W. Kolb, V.L. Teplitz, and R.V. Wagoner, Phys. Rev. D 17 (1978) 1529; J. Audouze, D. Lindley, and J. Silk, ApJ 293 (1985) 523. [20] E. Holtmann, M. Kawasaki, and T. Moroi, hep-ph/9603241 [21] G. Sigl, K. Jedamzik, D.N. Schramm, and V.S. Berezinsky, Phys. Rev. D 52 (1995) 6682. [22] M.H. Reno and D. Seckel, Phys. Rev. D 37 (1988) 3441. [23] S. Dimopoulos, R. Esmailzadeh, L.J. Hall, and G.D. Starkman, ApJ 330 (1988) 545.
Big Bang Nucleosynthesis With Small-Scale Matter-Antimatter Domains J.B. Rehm and K. Jedamzik Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str.1, D-85748 Garching Big Bang Nucleosynthesis (BBN) is one of the furthest back-reaching cosmological probes available. By means of comparing the predicted and observationally inferred light element abundances the physical conditions as early as a few seconds after the Big Bang can be scrutinized [1]. Nevertheless, presence of matter-antimatter domains during BBN on length scales comparable in size to the neutron diffusion length at temperatures between 10 and 10 −2 MeV (see e.g. [2]) has so far not been investigated. To our knowledge, the influence of antimatter on BBN has only been studied [3] with respect to a homogeneous injection of antiprotons into the primordial plasma after the end of BBN (T < 10 keV). The conclusion of such studies is that only a small fraction of about 10 −3 antiprotons per proton is allowed to be injected after the BBN epoch for the abundances of deuterium and 3 He produced in ¯p 4 He reactions not to exceed the observationally inferred values. In this work [4] we discuss the BBN in a baryo-asymmetric universe with a inhomogeneous distribution of matter-antimatter domains. For possible scenarios which may yield matterantimatter domains during an electroweak baryogenesis scenario see e.g. Refs. [5, 6]. As long as the diffusion length of neutrons and antineutrons is shorter than the size of a typical domain, matter and antimatter remain segregated. Note that proton diffusion is suppressed due to Coulomb scattering. Therefore, annihilations may likely only proceed when (anti)neutrons diffuse out of their domains. We identify three main scenarios: 1. Annihilations before weak freeze-out: No effect on the light-element abundances because the n/p-ratio, which governs the abundances, is reset to the equilibrium value by the fast weak interactions. 2. Annihilations between weak freeze-out (≈ 1 MeV) and the onset of 4 He synthesis (T ≈ 0.08 MeV): The n/p-ratio is strongly affected. Annihilation of antimatter mostly occurs on neutrons, since neutrons can both be annihilated by antineutrons diffusing into the matter region and diffuse themselves into the antimatter region to annihilate there on antiprotons and antineutrons. Protons on the other hand are confined to the matter region and can only be annihilated by diffusing antineutrons. By providing this effective sink for neutrons, the 4 He abundance may be substantially lower than in a standard BBN scenario at the same net entropy-per-baryon, simply because there are less neutrons left to build up 4 He. In extreme cases, when all neutrons have annihilated on antimatter before the onset of 4 He synthesis, zero net 4 He production results. This may well represent the only known BBN scenario in a baryo-asymmetric universe which precludes the production of any light elements. 3. Annihilations well after BBN: This scenario was already mentioned above. Annihilations of only small amounts of antimatter on 4 He may easily overproduce the cosmic deuterium and 3 He abundances. In summary, the figure illustrates that matter-antimatter domains present at the BBN epoch may have dramatic effects on the net synthesized 4 He abundance. By comparison, the abundances of other light isotopes are generally less affected. A more detailed analysis of BBN with matter-antimatter domains will be presented in a forthcoming work [4]. 147
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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
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 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
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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: some heating of the plasma. In cont
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 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
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196 C Astrophysics and Cosmology C1
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