A linear analysis of the radial pulsations of H-deficient stars

Details A linear analysis of the radial pulsations of H-deficient stars A linear analysis of the radial pulsations of H-deficient stars

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277.1393s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 4, pp. 1393-1398.

Astronomy and Astrophysics

Astronomy

24

Stars: Chemically Peculiar, Hertzsprung-Russell (Hr) Diagram, Stars: Individual: V652 Her, Stars: Individual: Lss 3184, Stars: Individual: Upsilon Sgr, Stars: Oscillations

Scientific paper

This paper presents results of a linear analysis of the radial pulsations (oscillations) of H-deficient stars, in which recently published OPAL opacity data were used. The classical kappa mechanism associated with the Fe opacity peak at T~2x10^5 K extends the instability region downward (like a `finger') around log T_eff~4.3 in the Hertzsprung-Russell (HR) diagram. The pulsations of V652 Her and LSS 3184, relatively less luminous helium stars, are attributed to the classical kappa mechanism. The strange modes caused by the opacity peak make envelopes with T_eff as high as 10^5K overstable if the luminosity is sufficiently high. Pulsating luminous H-deficient stars are located in the strange-mode instability region in the HR diagram. Their periods are more or less consistent with theoretical ones of overstable low-order radial modes for M~1 to ~0.7 M_solar. The pulsation period of the hydrogen-deficient binary upsilon Sgr is found to be consistent with models having a mass of ~3 M_solar, although its radius is larger than those predicted by evolutionary models for pure helium stars. The mass is high enough to be a progenitor of Type Ib supernovae.

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