A discussion of the eccentric binary hypothesis for transient X-ray sources. II - Gradual acceleration stellar wind model

Details A discussion of the eccentric binary hypothesis for transient X-ray sources. II - Gradual acceleration stellar wind model A discussion of the eccentric binary hypothesis for transient X-ray sources. II - Gradual acceleration stellar wind model

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980a%26a....90...44a&link_type=abstract

Astronomy and Astrophysics, vol. 90, no. 1-2, Oct. 1980, p.44-47. Research supported by the United States - Israel Binational S

Astronomy and Astrophysics

Astrophysics

10

Binary Stars, Eccentric Orbits, Stellar Models, Stellar Winds, X Ray Stars, Neutron Stars, Stellar Mass Accretion, Supergiant Stars

Scientific paper

The eccentric binary hypothesis for transient X-ray sources is examined in the framework of the gradual acceleration stellar wind model proposed by Barlow and Cohen (1977). It is found that a consideration of the ratio of maximum to minimum luminosities and of the ratio of the durations of the high and low states, for a typical transient X-ray source, yields a rather high eccentricity, despite the gradual acceleration of the wind. When typical physical parameters for the binary members are taken into account, it is found that a consistent description is possible only for very eccentric orbits (eccentricity greater than or equal to 0.9), thus the model is inadequate as a general explanation of the X-ray transient phenomenon. The recurrent transient X-ray source 4U 1630-47, which was considered in the past to be a realization of the eccentric binary model is studied, and it is demonstrated that it cannot be described consistently within the framework of the model, unless the optical primary is very peculiar.

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