Observation of a partial X-ray eclipse in the long-period low-mass X-ray binary 2S 0921-630

Details Observation of a partial X-ray eclipse in the long-period low-mass X-ray binary 2S 0921-630 Observation of a partial X-ray eclipse in the long-period low-mass X-ray binary 2S 0921-630

May 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.226..423m&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 226, May 15, 1987, p. 423-432. Research supported by th

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23

Accretion Disks, Eclipsing Binary Stars, Stellar Spectra, X Ray Binaries, Eclipses, Satellite Observation, Stellar Mass, Stellar Radiation

Scientific paper

A partial eclipse of the X-ray flux from 2S 0921-630 has been recorded for the first time, using the EXOSAT satellite. The time of the X-ray eclipse agrees with an extrapolation of the ephemeris of optical dips in 2S 0921-630, strongly supporting the hypothesis that 2S 0921-630 is an eclipsing binary with a period of just over 9 day. The X-ray eclipse lasts for over 1 day and has a smooth ingress and egress. At mid-eclipse the source flux drops to ≡30 per cent of its pre-eclipse value. The results of another, shorter, X-ray observation, also made at the predicted time of eclipse centre, suggest that the X-ray eclipse is a stable feature. The partial nature of the X-ray eclipse leads to the hypothesis that the binary companion in 2S 0921-630 obscures an extended medium which is scattering X-rays from a central, compact source into the line-of-sight. A simple model for the X-ray eclipse combined with optical radial velocity data suggests that the companion star in 2S 0921-630 is undermassive for its size compared to a normal, isolated star.

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