Proc. Neutrino Astrophysics - MPP Theory Group

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Contents History R.L. Mößbauer History of Neutrino Physics: Pauli’s Letters ......................................... 3 A. Dar What Killed the Dinosaurs? ........................................................ 6 Solar Neutrinos M. Stix Solar Models ...................................................................... 13 H. Schlattl, A. Weiss Garching Solar Model: Present Status .............................................. 19 M. Altmann Status of the Radiochemical Gallium Solar Neutrino Experiments .................. 22 Y. Fukuda (for the Superkamiokande Collaboration) Solar Neutrino Observation with Superkamiokande ................................. 26 M.E. Moorhead (for the SNO Collaboration) The Sudbury Neutrino Observatory ................................................ 31 L. Oberauer (for the Borexino Collaboration) BOREXINO ....................................................................... 33 M. Junker (for the LUNA Collaboration) Measurements of Low Energy Nuclear Cross Sections .............................. 36 G. Fiorentini Solar Neutrinos: Where We Are and What Is Next? ............................... 40 Supernova Neutrinos W. Hillebrandt Phenomenology of Supernova Explosions ........................................... 47 B. Leibundgut Supernova Rates ................................................................... 51 A.G. Lyne Pulsar Velocities and Their Implications ........................................... 54 W. Keil Convection in Newly Born Neutron Stars .......................................... 57 H.-Th. Janka Anisotropic Supernovae, Magnetic Fields, and Neutron Star Kicks ................. 60 K. Sato, T. Totani, Y. Yoshii Spectrum of the Supernova Relic Neutrino Background and Evolution of Galaxies .. 66 G.G. Raffelt Supernova Neutrino Opacities ..................................................... 73 v
Page 1 and 2: arXiv:astro-ph/9801320v1 30 Jan 199
Page 3: Preface This was the fourth worksho
Page 7 and 8: M. Bartelmann Neutrinos and Structu
Page 9: History
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
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48 Indirect information can be obta
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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
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