Diffusion-induced iron accumulations and thermohaline convection in A type stars : asteroseismic implications

Details Diffusion-induced iron accumulations and thermohaline convection in A type stars : asteroseismic implications Diffusion-induced iron accumulations and thermohaline convection in A type stars : asteroseismic implications

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011sf2a.conf..253t&link_type=abstract

SF2A-2011: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics Eds.: G. Alecian, K. Belkacem,

Astronomy and Astrophysics

Astrophysics

Stars:Abundances, Stars:Oscillations, Hydrodynamics, Convection, Asteroseismology

Scientific paper

The radiative acceleration on iron inside stars may lead to an accumulation of this element in stellar internal layers. This iron accumulation may have many important consequences. It may lead to an extra convective zone, and in some cases it may help triggering stellar pulsations. In this framework diffusion induced-iron accumulations are sometimes invoked to reconcile seismic observations and stellar modelling. These accumulations provide a natural answer to the κ-mechanism boost required to explain the mode excitation in several kind of pulsating stars (e.g. β Cephei, SPB, sdB stars). However, the computations which have been done up to now ignore an important effect: the double-diffusive or ``thermohaline'' convection induced by the inverse μ-gradients. Radiative diffusion and thermohaline convection have been introduced in the Toulouse-Geneva stellar evolution code. We present here stellar models computed in this context. We show how thermohaline convection modifies the iron profiles inside stars, with important consequences for the chemical stratification and the seismic properties of stars.

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