Proc. Neutrino Astrophysics - MPP Theory Group

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64 becomes neutron-rich. On the one hand, the unequal concentrations of neutrons and protons cause different opacities for νe and ¯νe, on the other hand the growing abundance of neutrons implies an increase of the total polarization of the nucleonic medium because the contributions from neutrons and protons have opposite signs and partly cancel. For a typical post-collapse composition, Yp ≈ 0.35 and Yn ≈ 0.65, this cancellation is severe and reduces the polarization to roughly 1/8 of the value for a neutronized medium with Yp ≈ 0.1 and Yn ≈ 0.9. The latter composition is representative of the late Kelvin-Helmholtz cooling phase after the deleptonization of the proto-neutron star. Most (60–90%) of the neutrino energy is radiated during this phase which is therefore decisive for a “rocket engine” effect by asymmetric neutrino emission. Of course, the estimated velocity in Eq. (2) is an upper limit which could be realized only if the interior magnetic field were uniform in the z-direction throughout the neutron star. Convective processes that reach deep into the star will certainly destroy the ordered structure of the field. In case of rapid rotation of the newly formed neutron star (rotation periods of a few milliseconds), however, convection can develop only near the equatorial plane but is suppressed near the rotation axis where an ordered field structure could persist in a large fraction of the neutron star volume. Conclusions If parity violation of weak interactions plays the crucial role to kick pulsars and if convection is important during the early phases of a neutron star’s life, one would therefore conclude that the observed velocities of fast pulsars between several 100km/s and more than 1000km/s require interior magnetic fields from a few 10 13 G to ∼ 10 14 G, and that the largest velocities might indicate rapid rotation of the newly formed neutron star. Acknowledgements This work was supported by the “Sonderforschungsbereich 375-95 für Astro-Teilchenphysik” der Deutschen Forschungsgemeinschaft. Stimulating discussions with S. Hardy, G. Raffelt, and S. Yamada are acknowledged. References [1] C. Fryer and V. Kalogera, preprint, astro-ph/9706031, subm. to Astrophys. J. (1997). [2] C. Fryer, A. Burrows, and W. Benz, preprint, subm. to Astrophys. J. (1997). [3] A. Burrows and J. Hayes, Phys. Rev. Lett. 76 (1996) 352. [4] M. Herant, W. Benz, W.R. Hix, C.L. Fryer, and S.A. Colgate, Astrophys. J. 435 (1994) 339. [5] H.-Th. Janka and E. Müller, Astron. Astrophys. 290 (1994) 496. [6] S.E. Woosley, in: The Origin and Evolution of Neutron Stars, IAU Symposium 125, eds. D.J. Helfand and J.-H. Huang (Kluwer, Dordrecht, 1987) 255. [7] A. Burrows, J. Hayes, and B.A. Fryxell, Astrophys. J. 450 (1995) 830. [8] C. Thompson and R.C. Duncan, Astrophys. J. 408 (1993) 194.
[9] G.S. Bisnovatyi-Kogan, Astron. Astrophys. Transactions 3 (1993) 287. [10] A. Kusenko and G. Segrè, Phys. Rev. Lett. 77 (1996) 4872. [11] E.Kh. Akhmedov, A. Lanza, and D.W. Sciama, preprint, hep-ph/9702436 (1997). [12] W. Keil, PhD Thesis, TU München (1997). [13] H.-Th. Janka and W. Keil, preprint, MPA-Report 1043, astro-ph/9709012 (1997). [14] E. Roulet, preprint, hep-ph/9711206, subm. to JHEP (1997). [15] C.J. Horowitz and Gang Li, preprint, astro-ph/9705126, subm. to Phys. Rev. Lett. (1997). [16] C.J. Horowitz and J. Piekarewicz, preprint, hep-ph/9701214 (1997). [17] H.-Th. Janka, talk at the ITP Conference on Supernova Explosions: Their Causes and Consequences, Santa Barbara, August 5–9, 1997, http://www.itp.ucsb.edu./online/supernova/snovaetrans.html. [18] D. Lai and Y.-Z. Qian, preprint, astro-ph/9712043, subm. to Astrophys. J. (1997). [19] H.-Th. Janka and G. Raffelt, in preparation (1998). 65
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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
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 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: Figure 1: Neutrino luminosity and e
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 118 and 119: 110 in gamma-rays. However, the acc
Page 120 and 121: 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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