Other
Scientific paper
Dec 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996mnras.283.1349k&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 283, Issue 4, pp. 1349-1354.
Other
13
Stars: Evolution, Stars: Individual: V652 Her, Stars: Oscillations, Stars: Variables: Other
Scientific paper
Some new timings of maxima of the pulsating hydrogen-deficient star V652 Her (BD+13 deg 3224) obtained during 1991-95 are reported. The data show that the ephemeris for times of maxima can no longer be represented by a cubic polynomial, and that a quartic term is necessary. The star could have brightened by up to 0.008 mag over the last decade, although this is not firmly established (the apparent change could also be due to small zero-point effects, for example). The shape of the light curve appears essentially unaltered over the same time interval; any changes are less than ~0.003 mag in size. Attempts have been made to understand the changing ephemeris in terms of changing stellar radius (R), mass (M) and pulsation constant (Q). A satisfactory match to the observations is obtained by a function including the first three derivatives of radius, R_solar, R_solar_solar and R & tdot;. The addition of a small mass-loss term does not significantly improve the fit. With the available data we cannot rule out (or distinguish between) small values of M_solar or Q_solar, but the values derived for the radius derivatives should stringently constrain pulsation models for V652 Her, and suggest extremely rapid evolution not yet accounted for in non-linear radial pulsation calculations.
Kilkenny Dave
Lynas-Gray Anthony E.
Roberts Gareth
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