Modelling compact pulsators

Details Modelling compact pulsators Modelling compact pulsators

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jphcs.118a2022r&link_type=abstract

Journal of Physics: Conference Series, Volume 118, Issue 1, pp. 012022 (2008).

Physics

Scientific paper

We currently know of five distinct classes of compact pulsators, loosely defined as oscillating stars with a surface gravity above log g = 5. Three of these fall into the white dwarf regime (GW Vir, V777 Her and ZZ Ceti stars), while the other two are identified with hot B subdwarfs (EC 14026 and PG 1716 stars). In all cases, the instabilities are thought to be associated with the partial ionisation of the envelope constituents. We discuss, for each type of pulsator, our current theoretical understanding of the observed instability strips as well as the details of the driving mechanism at work. In terms of attempts at a quantitative exploitation of the observed period spectra through asteroseismology, we focus on the particularly successful case of the rapidly pulsating subdwarf B (EC 14026) stars. So far, we have been able to constrain the fundamental stellar parameters for 12 targets. This is sufficient for first comparisons with different evolutionary scenarios, and will likely play a crucial part in an eventual understanding of the formation of these objects.

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