Proc. Neutrino Astrophysics - MPP Theory Group

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30 log(Δm 2 (eV 2 log(Δm )) 2 (eV 2 log(Δm )) 2 (eV 2 )) -3 -4 -5 -6 -7 -8 -4 -3.5 -3 -2.5 -2 -1.5 -1 -0.5 0 log(sin 2 -8 -4 -3.5 -3 -2.5 -2 -1.5 -1 -0.5 0 log(sin 2θ) 2 day and night 5bins -8 -4 -3.5 -3 -2.5 -2 -1.5 -1 -0.5 0 log(sin 2θ) 2 spectrum 2θ) log(Δm 2 (eV 2 log(Δm )) 2 (eV 2 )) -3 -4 -5 -6 -7 -8 -4 -3.5 -3 -2.5 -2 -1.5 -1 -0.5 0 log(sin 2 -8 -4 -3.5 -3 -2.5 -2 -1.5 -1 -0.5 0 log(sin 2θ) 2 day and night spectrum w/ flux constraint 2θ) Figure 4: (a) 95% C.L. excluded region in MSW parameters. Inside of solid and dotted line are excluded by the observed energy spectrum and the day/night flux difference, respectively. (b) Allowed region in MSW parameters with measured 8 B neutrino flux. Thick solid line, dashed line and thin solid line correspond to 95%, 90% and 68% C.L., respectively. Shaded region is allowed at 95% C.L. by Hata. References [1] To be submitted. [2] Y. Fukuda et al., Phys. Rev. Lett. 77, 1683 (1996). [3] J.N. Bahcall and M. Pinsonneault, Rev. Mod. Phys. 67, 781 (1995). [4] N. Hata and P. Langacker, IASSNS-AST 97/29, UPR-751T, hep-ph/9705339, May 1997. [5] S.P. Mikheyev and A.Y. Smirnov, Sov. Jour. Nucl. Phys. 42, 913 (1985); L. Wolfenstein, Phys. Rev. D17, 2369 (1978).
The Sudbury <strong>Neutrino</strong> Observatory M.E. Moorhead (on behalf of the SNO Collaboration) Particle and Nuclear Physics Laboratory, Keble Road, Oxford OX1 3RH, UK The Sudbury <strong>Neutrino</strong> Observatory (SNO) [1] is a 1,000 ton heavy water (D2O) Cherenkov detector in Sudbury, Ontario (Canada) which will start taking data in ‘98. The ν reactions which occur in D2O and the extremely low background environment of the detector will allow the following measurements: i) the νe and νx (flavour independent) fluxes, and their ratio, for 8 B solar ν’s, ii) the energy spectrum of 8 B νe’s above 5 MeV, iii) time dependence in the 8 B flux, and iv) detailed studies of the ν burst from a galactic supernova, including a search for νµ and ντ masses above 20 eV. For the 8 B solar ν measurements, the νe/νx flux ratio and the νe energy spectrum constitute two separate tests of ν oscillations which are both independent of solar model flux calculations [2]. If the currently favoured MSW solution [3] of the solar neutrino problem is correct then the νe/νx flux ratio should provide conclusive proof of oscillations with one year’s data yielding a 17 sigma departure from unity (statistical error only). The detector is situated two kilometers underground in a dedicated laboratory that has been excavated in the Creighton nickel mine of INCO Corporation. This laboratory comprises facilities for changing into clean-room clothing, a lunch room, a car wash for bringing equipment into the clean area, a utility room where the H2O and D2O systems are located, a control room and a 30 m × 23 m barrel shaped cavity for the detector itself. The walls of the cavity have been coated with concrete and low-activity Urylon, a water proof radon barrier. Inside this cavity is located a 12 m diameter spherical acrylic vessel (AV), recently completed, for containing the D2O neutrino target. Almost completely surrounding this AV, stands a 17 m geodesic sphere supporting 9,500 20-cm-Hamamatsu PMTs, each of which is equipped with a light reflecting concentrator to increase its effective photocathode area by a factor 1.7. Beginning in March ‘98, the detector will be filled with 7,000 tons of high purity H2O outside the acrylic vessel (to act as shielding for high energy gamma rays coming from the rock and the PMTs) and 1,000 tons of D2O inside the AV. The filling will take between 3–4 months and hence data taking will begin in mid-98. The event rates for solar ν’s, assuming the full SSM 8 B flux [4], and for a supernova (SN) at the center of our galaxy are given in Table 1. Apart from the neutral current (NC) reaction, all of the events are detected by the array of 9,500 PMTs via the Cherenkov radiation emitted by a single electron (or positron) of energy ≥ 5 MeV, the detector’s threshold. The NC reaction produces a free neutron in the D2O which can be detected, after thermalization, by observing a subsequent neutron capture reaction. There are three capture reactions of interest depending on what additives are placed in the D2O: i) Pure D2O: In the case of no additive there is a 30% probability of capture on deuterium, which produces a 6.25 MeV gamma. This gamma converts to electrons by Compton scattering and pair production, and the resulting Cherenkov light is detected by the PMTs. Five hundred events a year are expected above the detector’s 5 MeV threshold. ii) MgCl2: Dissolving 2 tons of MgCl2 in the D2O gives an 83% chance of neutron capture on 35 Cl which produces an 8.5 MeV gamma cascade. The higher efficiency and Q-value of this capture (c.f. capture on deuterium in the pure D2O case) increases the number of detected events by a factor of 5 to 2,500 per year. 31
Page 1 and 2: arXiv:astro-ph/9801320v1 30 Jan 199
Page 3: Preface This was the fourth worksho
Page 6 and 7: vi S.J. Hardy Quasilinear Diffusion
Page 8 and 9: viii
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 40 and 41: 32 Table 1: Neutrino event rates in
Page 42 and 43: 34 tank and sphere high purity wate
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
Page 52 and 53: 44 Figure 2: The difference between
Page 55 and 56: Phenomenology of Supernova Explosio
Page 57 and 58: Figure 2: Theoretical classificatio
Page 59 and 60: Supernova Rates Bruno Leibundgut Eu
Page 61 and 62: galaxies, however, and the statisti
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Page 71 and 72: Figure 1: Neutrino luminosity and e
Page 73 and 74: [9] G.S. Bisnovatyi-Kogan, Astron.
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Page 85 and 86: Assuming a saturated thermal distri
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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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