Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.194..429k&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 194, Feb. 1981, p. 429-437. Research supported by the Science Research
Astronomy and Astrophysics
Astronomy
26
Eclipsing Binary Stars, O Stars, Orbital Elements, Radial Velocity, Stellar Spectra, Subdwarf Stars, Companion Stars, Stellar Evolution
Scientific paper
Radial velocities from over 50 spectra have been used to determine the velocity curve of the primary of this unusual evolved eclipsing binary system.We ind the semi-amplitude of the velocity variation to be K1 = 32.5 ± 1.5 km s-1 and hence the semi-major axis of the primary orbit, α1 = (0.117 ± 0.005) × 106 km and the mass function, f(m) = 0.00093 ± 0.00013 solar masses. Solutions for a range of primary masses, 0.01 Msun ≤ M1 ≤ 10 Msun are computed and the best (in the sense of most internally consistent) indicates that the component masses are ˜M1 0.5Msun, M2 0.07Msun; the radii are R1- ≃ 0.2Rsun,R2≃0.1Rsun and the component separation is about 1.4Rsun.The secondary cannot be a white dwarf and is probably the core remnant of an evolved star after considerable mass loss in a "common envelope" phase of evolution.
Hill Philip W.
Kilkenny Dave
Penfold J. E.
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