Identification of high-mass x-ray binaries

Details Identification of high-mass x-ray binaries Identification of high-mass x-ray binaries

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002phdt........16m&link_type=abstract

Thesis (PhD). OPEN UNIVERSITY (UNITED KINGDOM), Source DAI-C 64/01, p. 178, Spring 2003, pages.

Computer Science

Scientific paper

This thesis addresses the problem of the identification of the optical companions to high mass X-ray binaries. The reddening free Q parameter is investigated as a general tool for spectral identification and with particular reference to early type stars and Be stars in particular. Q values are calculated for all possible combinations of three and four UBVRI waveband colour/colour diagrams and Q parameter versus spectral type diagrams presented for luminosity classes I and V and for two extinction laws. These were then employed on three transient X-ray sources and stars in their surrounding fields to test their relative effectiveness at isolating the X-ray binary companion stars. The conclusion is reached that only Q values involving U band data are useful for this task. The search for four particular objects is reported; SAX J2103 +4545, XTE J1858 +034, GS 1843 +00 and OAO 1657 -415. The investigations of SAX J2103 +4545 and XTE J1858 +034 proved inconclusive whereas GS 1843 +00 has been identified as a B0-B2 IV-Ve star. Two alternatives are proposed for the characteristics of the optical companion in the system OAO 1657 -415, that of a Be star whose circumstellar material was not in evidence at the time of the observations, or a B giant with an optically thick disc mimicking a larger radius at the time of the wide eclipse. It is suggested that the family of companions to such sources may be more complex than previously supposed and that, due to the changing characteristics of some, identification of companions to high mass X-ray binaries needs to be approached from a number of angles.

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