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Making a seismic solar model and an estimate of the neutrino fluxes

Published online by Cambridge University Press:  25 May 2016

H. Shibahashi  and
M. Takata
H. Shibahashi
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan
M. Takata
Affiliation:
Department of Astronomy, University of Tokyo, Bunkyo-ku, Tokyo 113, Japan

Abstract

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We present a method of making a solar model based on the helioseismic data. We first invert the observed eigenfrequencies to determine the sound speed profile, and then solve the basic equations governing the stellar structure with the imposition of the determined sound-speed profile. This approach is different from that of the standard solar model in the sense that the ‘seismic’ solar model is a snapshot model of the sun constructed without any assumption about the history of the sun. We invert the data obtained at the South Pole by the Bartol/NSO/NASA group along with BISON, HLH, and LOWL data. Finally we estimate the neutrino fluxes of the seismic model.

Type
Part II: Internal structure and rotation. Seismic inversions
Information
Symposium - International Astronomical Union , Volume 181: Sounding Solar and Stellar Interiors , 1997 , pp. 167 - 174
Copyright
Copyright © Kluwer 1997 

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