| Project/Area Number |
06452018
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| Research Category |
Grant-in-Aid for General Scientific Research (B)
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| Allocation Type | Single-year Grants |
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| Research Field |
Astronomy
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| Research Institution | The University of Tokyo |
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Principal Investigator |
SHIBAHASHI Hiromoto The University of Tokyo, Graduate School of Science, Associate Professor, 大学院理学系研究科, 助教授 (30126081)
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| Co-Investigator(Kenkyū-buntansha) |
KOBAYASHI Naoki Tokyo Institute of Technology, Faculty of Science, Research Associate, 理学部, 助手 (30272660)
OSAKI Yoji The University of Tokyo, Graduate School of Science, Professor, 大学院理学系研究科, 教授 (30011547)
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| Project Period (FY) |
1994 – 1995
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| Project Status |
Completed (Fiscal Year 1995)
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| Budget Amount *help |
¥7,400,000 (Direct Cost: ¥7,400,000)
Fiscal Year 1995: ¥2,200,000 (Direct Cost: ¥2,200,000)
Fiscal Year 1994: ¥5,200,000 (Direct Cost: ¥5,200,000)
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| Keywords | Sun ; internal Structure / Sun ; Oscillation / Helioseismology / Solar Neutrinos |
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| Research Abstract |
We deduce the density, pressure, temperature, and hydrogen profiles in the solar interior by solving the basic equations governing stellar structure with the imposition that the sound speed profile is that determined by helioseismic data of Libbrecht et al. (1990 ; AAA 52.080.103) and Jimenez et al. (1988 ; AAA 45.080.041). This approach is completely different from that of the standard solar model, and is based on more experimentally well-determined data. We solve the equations by requiring that the mass and the mean molecular weight at the surface match the solar mass and a certain fixed value, respectively, as the outer boundary conditions. Together with these conditions and the appropriate inner boundary conditions, these equations are reduced to a boundary value problem. We examine whether the luminosity at the surface matches the observed value. The error levels are estimated by a Monte Carlo simulation with Gaussian noise on the sound speed profile. The seismic model thus constructed marginally satisfies the luminosity condition, L (R_*)=L_*, at the 3sigma level. Using this seismic model satisfying L (R_*)=L_*, we estimate the neutrino fluxes, and find that the ^8B neutrino flux is about 60% of that of the standard solar model. This model seems consistent with the Kamiokande neutrino detection experiment. The ^7Be neutrino flux of the model is about 20% smaller than the standard solar model, and the pp-neutrino flux of the model is almost the same as that of the standard solar model. We estimate the total neutrino capture rate of the chlorine experiment (Homestake) that of the gallium experiments (GALLEX and SAGE) but for a contribution from the CNO cycle by scaling the capture rates based on the standard solar model. The capture rates thus estimated are 5.62 SNU and 117 SNU,respectively, and they are higher than the observations by the 3sigma error level.
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