- Page 1 and 2: arXiv:astro-ph/9801320v1 30 Jan 199
- Page 3: Preface This was the fourth worksho
- Page 6 and 7: vi S.J. Hardy Quasilinear Diffusion
- Page 8 and 9: viii
- Page 12 and 13: 4 Pauli’s Letters Brief an Oskar
- Page 14 and 15: 6 What Killed The Dinosaurs? Arnon
- Page 16 and 17: 8 continental coasts. The spread of
- Page 18 and 19: 10 References [1] M.J. Benton, Scie
- Page 21 and 22: Solar Models M. Stix Kiepenheuer-In
- Page 23 and 24: the outer convection zone. As for t
- Page 25 and 26: Convective Overshoot and Magnetism
- Page 27 and 28: Garching Solar Model: Present Statu
- Page 29 and 30: Acknowledgments We would like to th
- Page 31 and 32: The combined result of all 65 Galle
- Page 33 and 34: long-term operation covering at lea
- Page 35 and 36: The variation of the water transpar
- Page 37 and 38: data/SSM BP95 1.2 1 0.8 0.6 0.4 0.2
- Page 39 and 40: The Sudbury Neutrino Observatory M.
- Page 41 and 42: BOREXINO L. Oberauer (for the Borex
- Page 43 and 44: procurement in batch mode. Given fu
- Page 45 and 46: limit Ue=240 eV. Thus, improved low
- Page 47 and 48: these cycles are scarcely known at
- Page 49 and 50: Table 1: The proposed solutions, th
- Page 51 and 52: Figure 1: The 8 B and 7 Be+CNO neut
- Page 53: Supernova Neutrinos
- Page 56 and 57: 48 Indirect information can be obta
- Page 58 and 59: 50 a single supernova seen in a neu
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52 there is a subdivision into thre
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54 Pulsar Velocities and Their Impl
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56 population which has remained gr
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58 a b Figure 1: Panel a shows the
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60 Anisotropic Supernovae, Magnetic
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62 scopic asymmetry can build up be
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64 becomes neutron-rich. On the one
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66 Spectrum of the Supernova Relic
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68 signal would provide a new test
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70 Figure 2: Cumulative numbers (i.
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72 Figure 4: Expected event rates a
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74 A controlled determination of th
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76 Assuming this maximum turbulence
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78 References [1] J. Nieves and P.B
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80 The damping coefficient consists
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82 for µe = 200 MeV and � �
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84 ❅ ✗✔ ❅❅■ ❅✄ �
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86 Photon Dispersion in a Supernova
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Gamma-Ray Bursts
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92 galaxy—see discussion below).
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94 Figure 2: The slope of the diffe
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96 Gamma-Ray Bursts: Models That Do
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98 of the engine itself). A longer
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100 Acknowledgements We thank Alexa
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102 to 100MeV < T < 0.01MeV and 2.9
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104 exceeds a few 10 49 erg. Even w
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106 Physical Processes Near Black H
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Astrophysical Sources of High-Energ
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A third, more speculative class of
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detectors search for horizontal sho
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[13] A. Dar and N.J. Shaviv, Astrop
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calibration is estimated to be ±2.
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Data Monte Carlo total νe CC νµ
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Neutrino Astronomy with AMANDA Ch.
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Thus an Amanda optical module consi
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Entry 10 3 10 2 10 1 No fake for co
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High Energy Neutrino Astronomy with
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test strings at the Toulon site and
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Figure 1: Typical Čerenkov telesco
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Galactic cosmic-ray electrons (whic
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[6] Proc. 25th ICRC (Durban): J. Qu
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Cosmology
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140 subtraction requires considerab
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142 i) Inhomogeneity in the Baryon-
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144 possibility seems to be ruled o
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146 References [1] R.V. Wagoner, W.
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148 4 He mass fraction fraction fra
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150 where I have ignored the cosmol
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152 We can therefore calculate thei
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154 In other words, the fast radiat
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156 Figure 2: The comoving free-str
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158 • Rapid radiation-driven expa
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Neutrino Experiments with Cryogenic
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produced in the target by neutrino
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OMNIS—A Galactic Supernova Observ
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The proposed detector array is refe
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a cosmologically-significant neutri
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to neutrino masses that vanish as t
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g 10 -3 10 -4 10 -5 1 10 m(ν τ )
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Figure 6: Supernovae shock reheatin
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[18] For a recent ref. see S. Hanne
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2030: Neutrino Thermometer Now we
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[7] For this point, as well as a lo
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Monday, Oct. 20: Solar Neutrinos 10
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Thursday, Oct. 23: High Energy Neut
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Arnon Dar Department of Physics and
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Matthias Junker Laboratori Nazional
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Marisa Sarsa Technische Universitä
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Our Sonderforschungsbereich (SFB)
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B Theoretical Particle Physics and