The Asteroseismic Analysis of the EC14026 Star PG 0014+067 Revisited

Details The Asteroseismic Analysis of the EC14026 Star PG 0014+067 Revisited The Asteroseismic Analysis of the EC14026 Star PG 0014+067 Revisited

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..334..619c&link_type=abstract

14th European Workshop on White Dwarfs, ASP Conference Series, Vol. 334 Proceedings of a meeting held at Kiel, July 19-23, 2004

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Scientific paper

We present a new detailed asteroseismological analysis of the rapid hot B subdwarf (sdB) pulsator -- or EC14026 star -- PG 0014+067 based on high signal-to-noise observations obtained in August 1999, with the Montréal three-channel photometer Lapoune used in conjunction with the Canada-France-Hawaii 3.6 m Telescope. These data offer a significant improvement in terms of coverage compared to the light curves used in Brassard et al. (2001). We apply a global optimization technique to isolate a model that best fits simultaneously all the observed periods of PG 0014+067, leading to the asteroseismic determination of the fundamental parameters of that star. Our new analysis yields results similar to those uncovered in Brassard et al. (2001) and thus confirms the conclusions drawn in that paper.

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