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About Seismological Properties of Intermediate Mass Stars

Published online by Cambridge University Press:  12 April 2016

N. Audard  and
J. Provost
N. Audard
Affiliation:
Département Cassini, Observatoire de la Côte d’Azur, BP 229, 06304 Nice cedex 4, France
J. Provost
Affiliation:
Département Cassini, Observatoire de la Côte d’Azur, BP 229, 06304 Nice cedex 4, France

Abstract

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Stars more massive than about 1.2M⊙ are characterised by a convective core, which induces at its frontier a rapid variation of the sound speed and of the Brunt-Väissälä frequency, close to a discontinuity. We present preliminary results about the search of the signature this core could have on the p-mode spectra. For a set of frequencies of three stars of 1, 1.5 and 2 M⊙, we study in particular the small frequency separation Δν0,2, ~ νn,l, νn-1,l+2 for high order and low degree oscillation modes, which is particularly sensitive to the interior of stars. We underline characteristic behaviours of the 1.5 and 2 M⊙ stars, through the comparison between computed frequencies and their approximation obtained by asymptotic and polynomial fittings, and also through second order quantities relatively to the frequencies.

Type
VI. Asteroseismology: theory
Information
International Astronomical Union Colloquium , Volume 137: Inside the Stars , 1993 , pp. 544 - 546
Copyright
Copyright © Astronomical Society of the Pacific 1993

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