Radial velocity curves of nine sdB binary stars

Details Radial velocity curves of nine sdB binary stars Radial velocity curves of nine sdB binary stars

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004ap%26ss.291..315e&link_type=abstract

Astrophysics and Space Science, v. 291, Issue 3, p. 315-319 (2004).

Astronomy and Astrophysics

Astrophysics

5

Subdwarfs, Binary

Scientific paper

Radial velocity curves have been measured for nine sdB stars from high resolution optical spectra and are found to be sinusoidal indicating that they are binary stars with circular orbits. Their periods range from ≈12 h to more than 8 days. The companions are invisible in optical light. Minimum companion masses are derived from the mass functions, assuming the mass of the sdB primary to be half a solar mass. We argue that the companions to UVO 1735+22, Feige 108, HD 188112, and HD 171858 are white dwarfs, since their (statistically) most likely mass is above ≈0.7M &sun;. Five of the systems have not been investigated before, for the others our results agree with previously published ones.

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