FUSE Observations of PG 1716+426 stars

Details FUSE Observations of PG 1716+426 stars FUSE Observations of PG 1716+426 stars

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99s.133b&link_type=abstract

Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.133

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Scientific paper

The PG 1716+426 stars are pulsating subdwarf B stars known to exhibit very low amplitude (= 5 mmag), long-period (2000-8000 s), multiperiodic luminosity variations. These variations are associated with high radial order g modes. In the PG 1716+426 stars, the k driving mechanism is currently thought to be similar to that which is relevant to the hotter, shorter-period EC 14026 stars. The driving is linked to an opacity bump associated with a local enhancement of the abundance of iron and, presumably, other iron-peak elements in the envelope brought about by radiative element support. The PG 1716+426 stars might represent an ideal testing ground for this model, as they have cooler temperatures and likely lower stellar-wind mass-loss rates than the EC 14026 stars. In this work, we describe a set of FUSE spectra secured with the aim of testing these ideas, and provide a preliminary analysis of the abundances of iron peak elements in the sample of five PG 1716+426 stars observed to date.

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