Gravity-mode pulsations in subdwarf B stars: a critical test of stellar opacity

Abstract

The identification of non-radial g-mode oscillations as the cause of variability in cool subdwarf B stars (PG1716 variables) has been frustrated by a 5 000 K discrepancy between the observed and theoretical blue edge of the instability domain (Fontaine et al. 2003). A major component in the solution to this problem has been identified} by (a) using updated OP instead of OPAL opacities and (b) considering an enhancement of nickel, in addition to that of iron, in the driving zone. The reason for this success is that, in OP, the ``Fe-bump'' contributions from iron and nickel occur at higher temperatures than in OPAL. As well as pointing to a solution of an important problem in stellar pulsation theory, this result provides a critical test for stellar opacities and the atomic physics used to compute them.

4 figures, 2 tables, accepted for publication in MNRAS (Letters)

References in corpus (1)

• Fe-bump instability: the excitation of pulsations in subdwarf B and other low-mass stars

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