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Seismic Solar Models and the Neutrino Problem

Published online by Cambridge University Press:  08 February 2017

M. Takata  and
H. Shibahashi
M. Takata
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0032, Japan
H. Shibahashi
Affiliation:
Department of Astronomy, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0032, Japan

Abstract

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We determine the structure of the solar radiative zone with the imposition of the sound speed profile and the depth of the convection zone obtained from helioseismic analysis. We discuss the neutrino fluxes and capture rates using the resultant seismic solar model. We find that the seismic solar model cannot resolve the solar neutrino problem. The hydrogen and helium profiles of the Sun are obtained as a part of the solutions. We find that hydrogen is reduced in the core as expected in the theory of stellar evolution.

Type
I. Global Structure and Evolution of the Solar and Stellar Interior
Information
Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 21 - 24
Copyright
Copyright © Kluwer 1998 

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