Proc. Neutrino Astrophysics - MPP Theory Group

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28 Events/day/kton/bin 0.3 0.25 0.2 0.15 0.1 0.05 SK 374day 6.5-20MeV 22.5kt ALL 0 -1 -0.5 0 0.5 1 cosθ sun Figure 2: (a) Angular distribution to the solar direction and (b) heliograph for 374.2 days data. The energy spectrum of observed neutrinos is shown in Fig. 3(a). In this figure, expected spectra of MSW small angle parameter and just-so parameter are also shown. At first sight, small angle solution has better fit than flat (no oscillation) and just-so solution, but it is not significant within an experimental error. The day and night flux difference is obtained by; D − N D + N = −0.031 ± 0.024(stat.) ± 0.014(syst.). If night data are divided into five bins, those differences are shown in Fig. 3(b). In this figure, typical day/night flux variation of the large angle and the small angle solutions are also shown. There is no significant difference in day/night fluxes in present observation. Also Fig. 3(c) shows the seasonal variation of solar neutrino fluxes. Each season is pile up among different years. Solid line corresponds to the expected variation from an eccentricity of the Sun orbit. Within experimental error, there is no seasonal variation in present analysis. Those results are also same ones from Kamiokande. Two flavor neutrino oscillation For astrophysical solution, it is generally difficult to explain the solar neutrino problem with the modification of SSM including the observations from helioseismology. On the other hands, the elementary particle solution using MSW neutrino oscillation [5] seems to be an excellent for explanation of the solar neutrino problem, because it can distort the spectra of solar neutrinos. Also MSW oscillation can give a effect in the day/night fluxes variation. As obtained by Fig. 3, our observed spectrum can be seen slightly as distorted one, but not seen in variance between day/night fluxes. Using these results, we can obtained the excluded region at 95% C.L. in MS diagram as shown in Fig. 4(a). If we take the constraint of measured 8 B solar neutrino flux, allowed region of 95%, 90% and 68% C.L. as shown in Fig. 4(b). From these figures, our results and the allowed region given by Ref. [4] are consistent in MSW oscillation analysis.
data/SSM BP95 1.2 1 0.8 0.6 0.4 0.2 0 7 8 9 10 11 12 13 14 15 MeV 8 B Solar <strong>Neutrino</strong> Flux (x10 6 /cm 2 /s) 4 3 2 1 0 JAN data/SSM BP95 1 0.9 0.8 0.7 0.6 0.5 0.4 0.3 0.2 0.1 SK 374day 6.5-20MeV 22.5kt FEB MAR APR MAY JUN JUL day night1 night2 night3 night4 night5 0 -0.2 0 0.2 0.4 0.6 0.8 1 AUG SEP OCT NOV DEC Figure 3: (a) Energy spectrum, (b) Day/Night flux variation and (c) seasonal variation of obtained solar neutrino signal. Summary In summary, solar neutrino observation in Superkamiokande has started since May 1996 and has already taken 374.2 days data. The observed 8 B solar neutrino flux is about 37% of the prediction from SSM(BP95) and it is almost consistent with the result from Kamiokande. Using LINAC calibration system, we can reduce the systematic errors related to the energy scale. Obtained energy spectrum is likely distorted and it is indicated that the new physical solution will be solved the solar neutrino problem. New challenge to lower threshold analysis (≥ 5 MeV) has been started. Present radioactive ( 222 Rn) level is about 3 mBq/m 3 , however, we will able to reduce that level to factor 1/5. Even though the present analysis, we have succeeded to extract solar neutrino signals from 5–6.5 MeV region. Those data will give a strong indication to the solution for the solar neutrino problem within a few years. 29
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 38 and 39: 30 log(Δm 2 (eV 2 log(Δm )) 2 (eV
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 73 and 74: [9] G.S. Bisnovatyi-Kogan, Astron.
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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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