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Test of a New Theory for Stellar Convection using Helioseismology

Published online by Cambridge University Press:  12 April 2016

L. Paternó ,
R. Ventura ,
V.M. Canuto  and
I. Mazzitelli
L. Paternó
Affiliation:
Istituto di Astronomia dell’Università di Catania, Italy
R. Ventura
Affiliation:
Osservatorio Astrofisico di Catania, Italy
V.M. Canuto
Affiliation:
NASA - Goddard Institute for Space Studies, New York, USA
I. Mazzitelli
Affiliation:
CNR - Istituto di Astrofisica Spaziale, Frascati, Italy

Abstract

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Two evolutionary models of the Sun have been tested using helioseismological data. The two models use the same input micro-physics (nuclear reaction rates, opacity, equation of state) and the same numerical evolutionary code, but differ in the treatment of turbulent convection. The first model employs the standard mixing - length theory of convection, while the second one employs a new turbulent convection model which overcomes some basic inconsistencies of the standard theory of convection.

The test rests on the calculation of p-mode eigenfrequencies and on the comparison with the helioseismological data.

The comparison shows an overall improvement of the eigenfrequencies calculated with the new model with respect to those calculated with the standard model, although it appears that both models still suffer from inaccuracies especially in the treatment of the surface layers.

Type
I. Setting the stage: Sun, Stars Galaxies and the Universe
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 63 - 65
Copyright
Copyright © Astronomical Society of the Pacific 1993

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