Proc. Neutrino Astrophysics - MPP Theory Group

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58 a b Figure 1: Panel a shows the absolute values of the convective velocity for a non-rotating PNS model 0.7 s after the start of the simulation in units of 10 8 cm/s. The computation was performed in an angular wedge of 180 ◦ assuming axisymmetry. Panel b displays the relative deviations of the lepton fraction Ylep from the angular means 〈Ylep〉 at each radius for t = 0.7 s. The maximum deviations are of the order of 50%. Lepton-rich matter rises while deleptonized material sinks in. Since convective activity continues for more than 1 s in a large region of the PNS, convective ν transport shortens the cooling and deleptonization timescales of the PNS compared to results of 1D simulations and enhances the calculated ν luminosities of the star by up to 65%. The latter can have important influence on the interpretation of the measured ν signal from SN 1987A and might change limits of various quantities in nuclear and elementary particle physics which have been derived from these measurements. Moreover, the enhancement of the ν fluxes can also have important consequences for the explosion mechanism of the supernova, because it aids ν-driven explosions. The faster deleptonization modifies the luminosity ratio of νe and ¯νe in such a way that the electron fraction Y ej e in the ν-heated SN ejecta will be raised during the first few 100 ms after core bounce, but it will be lowered for t > ∼ 1 s compared to 1D simulations. This might help to solve the severe problems of the nucleosynthesis in current models of Type-II supernovae which disregard long-lasting convective activities in the PNS. Finally, convection in the PNS causes stochastical asymmetries of the ν flux. In our calculation the resulting recoil accelerates the PNS to ∼ 9 km/s during 1.2 s (Fig. 2a). This is too small to explain measured proper motions of pulsars of a few 100 km/s. Both convective mass motions and anisotropic ν emission are a source of gravitational waves for
a b Figure 2: Panel a shows the recoil velocity of our PNS model in km/s as a function of time resulting from stochastical asymmetries in the ν flux. Panel b displays the spectral energy density of the emitted gravitational radiation caused by mass motions and anisotropic ν emission. more than 1 second (Fig. 2b). Most of the gravitational radiation is emitted at frequencies of 300–1400 Hz. Acknowledgements We thank S.W. Bruenn for kindly providing us with the post-collapse model used as initial model in our simulations. Support by the “SFB 375-95 für Astro-Teilchenphysik” of the German Science Foundation is acknowledged. References [1] M. Herant et al., ApJ 435 (1994) 339. [2] A. Burrows, J. Hayes, and B.A. Fryxell, ApJ 450 (1995) 830. [3] H.-Th.Janka and E. Müller, ApJ 448 (1995) L109. [4] H.-Th.Janka and E. Müller, A&A 306 (1996) 167. [5] A. Mezzacappa et al., ApJ, accepted (1997). [6] W. Keil, H.-Th. Janka, and E. Müller, ApJ 473 (1996) L111. [7] J.M. Lattimer and F.D. Swesty, Nucl. Phys. A 535 (1991) 331. [8] S.W. Bruenn, in Nuclear Physics in the Universe, eds. M.W. Guidry and M.R. Strayer, IOP, Bristol, (1993) 31. 59
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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
Page 15 and 16: Recent observations with the Hubble
Page 17 and 18: MACHO sample of ∼100,000 light cu
Page 19: Solar Neutrinos
Page 22 and 23: 14 In the depth range where an abun
Page 24 and 25: 16 as follows: (1) All the detector
Page 26 and 27: 18 [3] J.N. Bahcall and H.A. Bethe,
Page 28 and 29: 20 the opacity has a very slowly ch
Page 30 and 31: 22 Status of the Radiochemical Gall
Page 32 and 33: 24 known true source activity. The
Page 34 and 35: 26 Solar Neutrino Observation with
Page 36 and 37: 28 Events/day/kton/bin 0.3 0.25 0.2
Page 38 and 39: 30 log(Δm 2 (eV 2 log(Δm )) 2 (eV
Page 40 and 41: 32 Table 1: Neutrino event rates in
Page 42 and 43: 34 tank and sphere high purity wate
Page 44 and 45: 36 Measurements of Low Energy Nucle
Page 46 and 47: 38 Figure 1: The S(E) factor of 3 H
Page 48 and 49: 40 Solar Neutrinos: Where We Are an
Page 50 and 51: 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: Convection in Newly Born Neutron St
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
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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
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126 However, in order to operate th
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128 could be gravitationally captur
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130 Ground-Based Observation of Gam
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132 Figure 2: Sensitivities in unit
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134 Crab flux Figure 4: Gamma-ray f
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136
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Helium Absorption and Cosmic Reioni
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Non-Standard Big Bang Nucleosynthes
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) 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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