Proc. Neutrino Astrophysics - MPP Theory Group

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132 Figure 2: Sensitivities in units of photons cm −2 sec −1 of various existing and planned detectors for high and very-high energy gamma rays for various energies (full lines) or at the energy threshold (big dot). The numbers are for a total measuring time of 50 hours for devices with a small field of view and 1 year for devices with a field of view of 1 steradian or larger [satellites: EGRET (existing) and GLAST (planned) and the array MILAGRO (planned)]. WHIPPLE and HEGRA are existing telescopes, VERITAS and MAGIC proposed large future devices. STACEE, CELESTE and GRAAL are detectors which are currently being set up using the large mirror areas at solar power plants. The dotted line gives the extrapolation of a source spectrum from GeV to VHE energies (active galaxy Mkn 421). The arrows indicate the intensity of this source during various viewing periods (“VP”) of the EGRET satellite. Recent results This summer (1997) the Australian-Japanese CANGAROO collaboration announced detection of radiation above 2 TeV from the remnant of the supernova (SNR) of A.D. 1006 [7]. The detected flux was close to previous theoretical predictions [8] on the basis of the hypothesis that cosmic-ray electrons are accelerated by the shock front of SNRs. The accelerated electrons suffer inverse Compton scattering on the cosmological 3 K background radiation, which are then detected in the TeV range. This is strong experimental support for the idea that the
Galactic cosmic-ray electrons (which account for about 1 % of the total cosmic-ray flux at earth) are due to shock wave acceleration in SNRs. Perhaps this brings us near to a solution of the historic question of the origin of the main hadronic part of cosmic rays: it had long been speculated that all cosmic rays with energies below about 100 TeV are accelerated in SNRs. The VHE upper limits on the SNR G78.2+2.1 shown as an example in Fig. 3 [9] present a problem for this scenario, though. This SNR lies near a dense molecular cloud which should act as a “target” for the accelerated cosmic-rays, leading to the prediction of a copious production of VHE gamma-rays via the reaction p + p → π0 → 2 γ. It is seen that the upper limits from various experiments shown in Fig. 3 are below theoretical predictions in the mentioned scenario [9, 10]. This has recently led to a revival of speculations on an extragalactical origin of the main part of hadronic cosmic rays [11]. The active galaxy Mkn 501 at a distance of about 100 Mpc from earth showed a spectacular outburst of TeV radiation 1997 which was observed in detail by 5 different collaborations [12]. At the highest activity level in April 1997 the flux was about 40 times higher than during the discovery of the source in 1995. Figure 4 shows the light curve determined by the HEGRA telescope 1. This light curve is the most complete of all measured ones because data were also taken during moonshine. The outburst was also observed in the X-ray and optical region and these multiwavelength studies are especially valuable to discriminate between various models for the origin of the TeV radiation and to find the reasons for its fluctuation. The measured VHE spectra already allow interesting conclusions about the intensity of cosmological infrared background radiation field [13]. Interactions of VHE photons with cosmological background fields will allow a variety of cosmological studies unique to this wavelength range [14]. integral flux [cm -2 s -1 ] 10 -5 10 -6 10 -7 10 -8 10 -9 10 -10 10 -11 10 -12 10 -13 10 -14 10 -15 10 -5 EGRET 1995 Whipple 1997 HEGRA CT-System 1997 AIROBICC 1997 AIROBICC 1996 CASA-MIA 1995 CYGNUS 1995 10 -4 10 -3 10 -2 10 -1 theory prediction α=2.1 theory prediction α=2.3 1 10 10 energy [TeV] 2 10 3 Figure 3: Upper limits on VHE radiation from the SNR G78.2+2.1. Whipple and HEGRA are Čerenkov telescopes, AIROBICC, CASA-MIA and CYGNUS are arrays. It now seems likely that the detection of γ-rays from a satellite above 100 MeV (EGRET) is due to a pulsar. 133
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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
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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
Page 89 and 90: So far the damping rate corresponds
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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
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 134 and 135: 126 However, in order to operate th
Page 136 and 137: 128 could be gravitationally captur
Page 138 and 139: 130 Ground-Based Observation of Gam
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
Page 184 and 185: 176 [5] A. Joshipura and J. W. F. V
Page 186 and 187: 178 Some Neutrino Events of the 21s
Page 188 and 189: 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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