Proc. Neutrino Astrophysics - MPP Theory Group

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168 Table 1: Comparison of proposed OMNIS multi-target observatory with world detectors based on direct detection with water and scintillator targets. Approximate event numbers for each neutrino type shown for a supernova at 8 kpc. Target Fiducial Target Event Number Material Mass (tons) Elements νe ¯νe νµ,τ + ¯νµ,τ Combined Target & Detector: Super-Kamiokande H2O 32000 p, e, O 180 8300 50 LVD “CH2” 1200 p, e, C 14 540 30 MACRO “CH2” 1000 p, e, C 8 350 25 SNO H2O 1600 p, e, O 16 520 6 SNO a D2O 1000 d, e, O 190 180 300 Separated Target & Detector: OMNIS 200 t Scintillator NaCl (rock) “8000” Na, Cl 10 10 400 + Natural Rock Fe 4000 Fe 10 10 600 + Installed Targets Pb 4000 Pb 280 30 1000 Direct Interaction Total: 300 50 2000 With Scintillator “CH2” 200 p, e, C 2 70 5 a Heavy water target not available indefinitely estimated neutron production rates in salt rock, iron, and lead are 0.06, 0.15, 1 per ton for a supernova at 8 kpc. In addition, higher collection efficiency is possible from Fe and Pb due to lower absorption [6], giving them an effectiveness in the ratio 1 : 4 : 30. Thus lead is by far the most effective target to maximise event numbers, but the design must include a sufficient quantity of the other targets to provide information on mixing between mu/tau and electron neutrinos, based on the fact that this would enhance the charged current excitation in Pb but not in Fe or rock. Table 1 shows the event numbers of different neutrino types from principal world detectors, compared with those from the proposed OMNIS detector. Note that the neutron background from U/Th in the rock would not be significant compared with the signal burst, and for sites with depths > 600 m, the neutron background from muons would also be an order of magnitude below the signal. Thus the project is technically straightforward and based on conventional low-cost neutron detection technology. Neutron background is discussed in more detail in [6] where some discussion is also included on the enormously greater background problem for extra-Galactic supernova detection. For discrimination of supernova events from local neutron showers from cosmic ray muons, it is desirable to split the array between several underground caverns, and also between several world sites, also permitting estimates of supernova direction by arrival time differences. In conclusion the relatively low unit cost of the OMNIS scheme makes it possible to propose a dedicated Galactic supernova neutrino observatory, capable of observing the time profile of the mu and tau neutrino component. This would provide the first direct measurement of
a cosmologically-significant neutrino mass, and the use of several different target elements, in conjunction with the large electron antineutrino signal from SuperKamiokande would also provide data on the presence or absence of neutrino mixing on the Galactic distance scale. It could be designed to run largely unattended, with minimal maintenance, so would be a part-time activity for the participating groups, alongside other underground experiments. The current collaboration on this project involves groups from RAL, Manchester, Sheffield, Imperial College (for the UK Boulby Mine site) and UCLA, UCSD, Ohio, LLNL, LANL, UT-Dallas, PNL, for the US Carlsbad site, both sites in low activity salt rock and already containing suitable infra-structure installed for other purposes. First prototype modules could now be set up in these sites and funding is being sought for this. New collaborators would be welcome to strengthen the case for construction of the full array. Acknowledgments I acknowledge clarifying discussions with D.B. Cline, G.M. Fuller, J.R. Wilson, B. Cox, G. McLaughlin, J.D. Lewin, R.N. Boyd, F. Boehm, J. Kleinfeller, R. Marshall, W. Vernon, R. Shirato, A. Burrows, and C.K. Hargrove. References [1] D.B. Cline et al., Phys. Rev. D 50 (1994) 720. [2] S. Van den Bergh, G.A. Tammann, Ann. Rev. Astron. Astrophys. 29 (1991) 363. [3] D. Kielczewska, Int. J. Mod. Phys. D 3 (1994) 331. [4] A. Burrows, Ann. Rev. Nucl. Part. Sci. 40 (1990) 181. [5] D.B. Cline et al., Nucl. Phys. B 14A (1990) 348; Astro. Lett. Comm. 27 (1990) 403. [6] P.F. Smith, Astropart. Phys. 8 (1998) 27. [7] G.M. Fuller, B.S. Meyer, Ap.J. 376 (1991) 701; 453 (1995) 792 [8] C.K. Hargrove et al., Astropart. Phys. 5 (1996) 183. [9] G. McLaughlin, G.M. Fuller, in preparation 169
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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
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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-
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 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 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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Page 192 and 193: 184 Tuesday, Oct. 21: Supernova Neu
Page 194 and 195: 186 Michael Altmann Technische Univ
Page 196 and 197: 188 Paolo Gondolo Max-Planck-Instit
Page 198 and 199: 190 Patrizia Meunier Max-Planck-Ins
Page 200 and 201: 192 Torsten Soldner Technische Univ
Page 202 and 203: 194 A Experimental Particle Physics
Page 204: 196 C Astrophysics and Cosmology C1
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