Other
Scientific paper
Dec 1985
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...299..839c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 15, 1985, p. 839-844.
Other
38
Spectrum Analysis, Stellar Spectrophotometry, Supergiant Stars, X Ray Binaries, Angular Velocity, B Stars, H Alpha Line, Neutron Stars, Orbital Elements, Spectral Line Width, Stellar Luminosity, Stellar Mass Accretion, Stellar Winds
Scientific paper
Spectroscopic observations show that LS I + 65 010 deg, the counterpart of the X-ray source 2S 0114 + 650, optically resembles the supergiant X-ray binary systems rather than the Be-type systems. The orbital period is 11.588 + or - 0.003 d with maximum positive velocity occurring at JD 2,444,4134.3. It is not possible to decide whether the orbit is circular or whether it has a small eccentricity of 0.16 + or - 0.007, both fit the observations equally well. The mass function is 0.006 solar masses, implying a mass of approximately 18 solar masses, for the B0.5 supergiant if the neutron star has a typical mass. It is argued that the source is 2.5 kpc from the sun, implying that the log of the X-ray luminosity is approximately 34.5 ergs/s, and that this system shares characteristics of both the supergiant X-ray binaries and the Be systems. The X-ray source appears to be fuelled by accretion of material from the stellar wind of the primary star, rather than by Roche lobe overflow. This accounts for its low X-ray luminosity compared to other supergiant X-ray binary systems.
Cowley Anne Pyne
Crampton David
Hutchings John B.
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