Asteroseismic signatures of helium gradients in main-sequence A stars; application to the roAp star HD 60435

Free access article

Issue		A&A Volume 425, Number 1, October I 2004


Page(s)		179 - 185
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20047034

A&A 425, 179-185 (2004)
DOI: 10.1051/0004-6361:20047034

Asteroseismic signatures of helium gradients in main-sequence A stars; application to the roAp star HD 60435

S. Vauclair¹ and S. Théado^{1, 2}

¹ Université Paul Sabatier, Observatoire Midi-Pyrénées, CNRS/UMR5572, 14 av. E. Belin, 31400 Toulouse, France
e-mail: svcr@obs-mip.fr
² Centro de Astrofisica da Universidade do Porto, rua das Estrelas, 4150-762 Porto, Portugal

(Received 8 January 2004 / Accepted 28 May 2004)

Abstract
Asteroseismology is found to be a excellent tool for detecting diffusion-induced helium gradients inside main-sequence A stars. Models have been computed for 1.6 and 2.0 $M_{\odot}$ stars with pure helium diffusion, at different ages, so that the helium gradient lies at different depths inside the star. The adiabatic oscillation frequencies have been analysed and compared with those of a model without diffusion. Clear signatures of the diffusion-induced helium gradient are found in the so-called "second differences": these frequency differences present modulations due to the partial reflexion of the sound waves on the layer where the helium gradient occurs. A tentative application to the roAp star HD 60435, which presents enough detected oscillation frequencies for the test to be possible, is very encouraging. The results suggest the presence of a helium gradient inside the star, which is consistent with the idea that the triggering of the oscillations is due to the hydrogen $\kappa$ -mechanism.

Key words: stars: oscillations -- stars: abundances -- diffusion -- stars: chemically peculiar

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