The Far-UV Spectrum of a Wind-Fed X-Ray Binary: LMC X-4 Seen with FUSE

Details The Far-UV Spectrum of a Wind-Fed X-Ray Binary: LMC X-4 Seen with FUSE The Far-UV Spectrum of a Wind-Fed X-Ray Binary: LMC X-4 Seen with FUSE

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...19713007b&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #130.07; Bulletin of the American Astronomical Society, Vol. 33, p.715

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Observations of the far UV spectrum of the X-ray binary LMC X-4 with the Lyman Far Ultraviolet Spectroscopic Explorer (FUSE) show a P Cygni O 6λ λ1031 .9,1037.6 doublet that varies over the 1.4 day orbit, due to the photoionization of the stellar wind by the X-rays from the neutron star. We observed from orbital phase φ =0.5, when the absorption was weakest, to φ =0.0, when the absorption was strongest. We investigate the structure of the stellar wind from the P Cygni line variability. Other absorption lines detected (Si 4λ λ1122 .5,1128.3, C 3λ1175 .7, P 5λ λ1118 ,1128, S 4λ λ1062 .7,1073.0) show only a velocity shift over half the binary orbit and are probably photospheric in origin. The line profiles are consistent with a stellar rotation velocity of 170 km s-1, the value found previously from optical spectroscopy, implying that the star rotates with twice the binary period. Simultaneous X-ray observations with the Rossi X-ray Timing Explorer (RXTE) show that an X-ray flare occurred during the FUSE observation. We search for an effect of the increased X-ray luminosity on the stellar continuum and the lines from the stellar wind.

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