Proc. Neutrino Astrophysics - MPP Theory Group

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Proceedings of the Fourth SFB-375 Ringberg Workshop “Neutrino Astrophysics” Sonderforschungsbereich 375 Research in Astro-Particle Physics E-mail: depner@e15.physik.tu-muenchen.de Postal Address: Technische Universität München Physik Department E15 — SFB–375 James-Franck-Straße D–85747 Garching Germany c○ Sonderforschungsbereich 375 and individual contributors Published by the Sonderforschungsbereich 375 Technische Universität München, D–85747 Garching January 1998
Preface This was the fourth workshop in our series of annual “retreats” of the Sonderforschungsbereich Astroteilchenphysik (Special Research Center for Astroparticle Physics), or SFB for short, to the Ringberg Castle above Lake Tegernsee in the foothills of the Alps. These meetings are meant to bring together the members of the SFB which are dispersed between four institutions in the Munich area, the Technical University Munich (TUM), the Ludwig- Maximilians-University (LMU), and the Max-Planck-Institute for Physics (MPP) and that for Astrophysics (MPA). We always invite a number of external speakers, including visitors at our institutions, to complement the scientific program and to further the exchange of ideas with the international community. This year’s topic was “Neutrino Astrophysics” which undoubtedly is one of the central pillars of astroparticle physics. We focused on the astrophysical and observational aspects of this field, deliberately leaving out theoretical particle physics and laboratory experiments from the agenda. Each day of the workshop was dedicated to a specific sub-topic, ranging from solar, supernova and atmospheric neutrinos over high-energy cosmic rays to the early universe. A session on future prospects served to conclude the workshop and provide an outlook on the field in the next decade and beyond. We started every topical session with one or two introductory talks, reviewing the status of theory and experiment and to providing some background for the non-experts. For the entire program we interpreted “neutrino astrophysics” in a broad sense, including, for example, the physics of γ-ray bursts or the recent observations of TeV γ-rays by the imaging air-Cherenkov technique. Some of the after-dinner-talks went significantly beyond a narrow interpretation of the field! From our perspective the profile of neutrino astrophysics as defined by our program worked very well, even better than we had hoped. We are proud that the main complaint of the participants seemed to be that they did not get enough mountain-hiking done because the sessions were too interesting to miss. Besides regular SFB resources this workshop was made possible by a direct grant from the Max-Planck-Society and additional funds from the Max-Planck-Institute for Astrophysics. Special thanks go to the SFB secretary, Maria Depner, for her smooth and skillful management of all practical matters related to the workshop. We thank the participants for their high-level contributions and for being extremely cooperative in submitting the “extended abstracts” of their talks on time and in a format that allowed us to produce these proceedings in electronic form. Anyone interested in a printed version should write to the SFB secretary at the address given on the previous page. We hope that you will find this booklet a useful and up-to-date resource for the exciting and fast-developing field of neutrino astrophysics. Michael Altmann, Wolfgang Hillebrandt, Hans-Thomas Janka and Georg Raffelt Munich, January 1998 iii
Page 1: arXiv:astro-ph/9801320v1 30 Jan 199
Page 6 and 7: vi S.J. Hardy Quasilinear Diffusion
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Page 11 and 12: History of Neutrino Physics: Pauli
Page 13 and 14: 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
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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
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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
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[7] Lilly, S., in Critical Dialogue
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) Phase Transitions in Neutron Star
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after the collapse began (nb., no e
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Models of Coalescing Neutron Stars
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Figure 2: Contour plots of the mass
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From our torus models we find that
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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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