Proc. Neutrino Astrophysics - MPP Theory Group

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126 However, in order to operate the detector and perform the installation within a reasonable time (5 years) additional logistic costs have to be taken into account. These are mainly the costs of modernisation the drilling equipment, a new building, fuel, cargo and technical personal. These support costs can be estimated to about 10 M$ [4]. Adding the costs of AMANDA-B and AMANDA-II, the ICECUBE detector would cost of the order of 50 M$ [4]. It is planned to start the installation in the beginning of year 2001 and finish it by 2005. A workshop on the ICECUBE project will be held in March 1998 [5]. References [1] F.Halzen: The AMANDA Neutrino Telescope: Science Prospects and Performance at first light. MADPH-97-1007, Univ. of Wisconsin, Madison, July 1997. [2] F.Halzen: Large natural Cherenkov Detectors: Water and Ice, TAUP-97, Gran Sasso, Sept. 1997. MADPH-97-1026, Univ. of Wisconsin, Madison, November 1997. [3] Contributions of the AMANDA collaboration to the 26th International Cosmic Ray Conference, Durban, South Africa, July 1997. [4] Biron et al.: Upgrade of AMANDA-B towards AMANDA-II, Proposal submitted to the DESY Physics Research Committee, June 1997. [5] ICECUBE, Neutrino Detector Workshop, 27-28 March 1998 http://www.ps.uci.edu/˜icecube/
High Energy Neutrino Astronomy with ANTARES M.E. Moorhead (for the ANTARES Collaboration) University of Oxford, Particle and Nuclear Physics Laboratory, Keble Road, Oxford OX1 3RH, UK Neutrino astrophysics has already generated considerable interest in both the particle physics and astrophysics communities, through the detection of solar neutrinos, atmospheric neutrinos and neutrinos from supernova 1987A. ANTARES [1] aims to extend this scientific reach to higher energies (10 GeV–10 PeV) where potential neutrino sources include Active Galactic Nuclei, Gamma Ray Bursters, pulsars, X-ray binaries, young supernovae remnants and neutralino annihilation in the center of the Sun or Earth. These neutrino observations should provide complementary information that might be difficult or even impossible to obtain through gamma or cosmic ray observations. The observable energy range for neutrinos extends well above 1–10 TeV where extra-galactic gamma rays are severely attenuated over cosmic distances by their interactions with infra red and cosmic microwave background photons. Moreover, unlike charged cosmic rays, neutrinos are not deflected by magnetic fields and thus point back to their source. There are several potential astrophysical sites for accelerating cosmic rays up to the energies of 10 20 eV that have been observed. In general, these sites will also produce significant fluxes of neutrinos and gamma rays through the decays of charged and neutral pions, which are produced in approximately equal numbers through soft interactions of the high energy protons with other protons or photons present in the acceleration site. The emitted fluxes of neutrinos and gamma rays from this mechanism would thus be roughly equal, however the gamma rays may be severely attenuated at the source by interactions with matter or photons, leaving the neutrinos as the best probe of the physics. Several authors (see [2] and references therein) have constructed models which account for the observed TeV gamma ray emission of Active Galactic Nuclei (AGNs) in terms of proton acceleration in the jets which emerge from the central black hole of 10 6 –10 10 solar masses. These authors predict between 100 and 1000 events per year from all AGNs in a neutrino detector with 1 km 2 effective area. Another possible cosmic acceleration site is the expanding fireball produced by coalescing neutron stars immediately after merging. These events are sufficiently energetic and numerous to explain the cosmic origin of the observed Gamma Ray Bursts (GRBs). Waxman and Bahcall [3] predict between 30–100 neutrino events per km 2 per year. Pulsed neutrino sources such as GRBs are easier to detect since the background from atmospheric neutrinos is greatly reduced by looking for time and direction coincidences with gamma-ray observations of GRBs with satelite experiments. They also offer the possibility of kinematic neutrino mass tests through the relative times of the neutrino and gamma signals at the Earth. Potential galactic acceleration sites of cosmic rays include pulsars, X-ray binaries and young supernova remnants. Calculations show that for these Galactic sources, total proton luminosities of a few percent of the Eddington limit could be detected by a km 2 neutrino detector. A very interesting signal for ANTARES arises if the non-baryonic dark matter is primarily in the form of weakly interacting massive particles, the favoured particle physics candidate being the lightest supersymmetric particle (LSP), normally assumed to be the neutralino (χ). A relic neutralino undergoing an elastic scatter while passing through a star or planet 127
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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
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14 In the depth range where an abun
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16 as follows: (1) All the detector
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18 [3] J.N. Bahcall and H.A. Bethe,
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20 the opacity has a very slowly ch
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22 Status of the Radiochemical Gall
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24 known true source activity. The
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26 Solar Neutrino Observation with
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28 Events/day/kton/bin 0.3 0.25 0.2
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30 log(Δm 2 (eV 2 log(Δm )) 2 (eV
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32 Table 1: Neutrino event rates in
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34 tank and sphere high purity wate
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36 Measurements of Low Energy Nucle
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38 Figure 1: The S(E) factor of 3 H
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40 Solar Neutrinos: Where We Are an
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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
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
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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
Page 122 and 123: 114 Today, however, charm productio
Page 124 and 125: 116 Atmospheric Neutrinos in Super-
Page 126 and 127: 118 number of events 300 200 100 (a
Page 128 and 129: 120 Acknowledgements D.K. is suppor
Page 130 and 131: 122 Key signatures for νµ nucleon
Page 132 and 133: 124 (a.u) 0.5 0.4 0.3 0.2 0.1 0 0 1
Page 136 and 137: 128 could be gravitationally captur
Page 138 and 139: 130 Ground-Based Observation of Gam
Page 140 and 141: 132 Figure 2: Sensitivities in unit
Page 142 and 143: 134 Crab flux Figure 4: Gamma-ray f
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Page 147 and 148: Helium Absorption and Cosmic Reioni
Page 149 and 150: Non-Standard Big Bang Nucleosynthes
Page 151 and 152: ) Non-standard Neutrino Properties
Page 153 and 154: some heating of the plasma. In cont
Page 155 and 156: Big Bang Nucleosynthesis With Small
Page 157 and 158: Neutrinos and Structure Formation i
Page 159 and 160: Photon and Neutrino Backgrounds The
Page 161 and 162: The (photon) temperature at aeq is
Page 163 and 164: spectrum has therefore changed to 1
Page 165 and 166: Figure 4: Growth of structure in CD
Page 167: Future Prospects
Page 170 and 171: 162 Figure 1: Calorimetric β − s
Page 172 and 173: 164 References [1] F. Gatti: Procee
Page 174 and 175: 166 The frequency of Galactic super
Page 176 and 177: 168 Table 1: Comparison of proposed
Page 178 and 179: 170 Neutrinos in Astrophysics José
Page 180 and 181: 172 N eq 7 6.5 6 5.5 5 4.5 4 3.5 3
Page 182 and 183: 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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