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Astron. Astrophys. 327, 349-360

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Updated solar models

P. Morel1, J. Provost1, and G. Berthomieu1

Département Cassini, UMR CNRS 6529, Observatoire de la Côte d'Azur, BP 4229, F-06304 Nice Cedex 4, France

Received 21 March 1997 / Accepted 26 May 1997


Solar models computed with mass loss, microscopic diffusion of helium and heavy element, and with updated physics have been evolved from the pre-main sequence to present day; they are compared to the observational constraints including lithium depletion and to the seismic reference model of Basu et al. (1996), derived by inversion. Microscopic diffusion significantly improves the agreement with the observed solar frequencies and agree with the seismic reference model within FORMULA for the sound velocity and FORMULA for the density, but slightly worsens the neutrino problem. Neither microscopic diffusion nor overshooting explain the observed lithium depletion consistently with helioseismological constraints, while a mass loss process does it. Models computed with OPAL equation of state and opacities are in a better agreement with the seismic sound speed. To reach the level of precision of helioseismological observations the accuracy of solar models still needs to be improved by one order of magnitude; any such improvement will necessitate equation of state and opacity data taking into account of detailed changes in the mixture.

Key words: Sun: abundances - Sun: evolution - Sun: oscillations - Sun: interior

Send offprint requests to: P. Morel, morel@obs-nice.fr

© European Southern Observatory (ESO) 1997

Online publication: October 1, 1997
Last change: April 8, 1998