Multisite campaign on HE0230-4323

Details Multisite campaign on HE0230-4323 Multisite campaign on HE0230-4323

Aug 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008noao.prop...35k&link_type=abstract

NOAO Proposal ID #2008B-0035

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Scientific paper

HE0230-4323 is a binary star with a 10.8 hour period (Edelman et al. 2005, Koen 2007). The primary is an ultraviolet-bright subdwarf B (sdB) star; the companion is invisible in the optical and is probably a late M/ brown dwarf. The primary is a pulsating variable, showing several frequencies in the range 8-60 cycles/day (periods of 25 minutes to 3 hours, see Fig. 1). The periods are anomalous - pulsation theory predicts that an sdB star this hot (T_eff=31550 K) should be a rapid pulsator (typical periods ~ 3 minutes). A further very strange feature of the pulsations is that variations through B and V filters have a 180 degree phase difference (Fig. 2). The frequency content of the pulsation spectrum appears to vary on a timescale of a day/few days. Extensive observations of the star will be used to constrain the physical properties of the star through asteroseismological modelling.

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