Rapid variability of P Cygni lines in massive X-ray binaries

Details Rapid variability of P Cygni lines in massive X-ray binaries Rapid variability of P Cygni lines in massive X-ray binaries

Jun 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...317..746k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 317, June 15, 1987, p. 746-749.

Astronomy and Astrophysics

Astrophysics

10

B Stars, Early Stars, O Stars, Spectral Line Width, Stellar Spectra, X Ray Binaries, Iue, Stellar Winds, Ultraviolet Spectra, Variability

Scientific paper

In early-type X-ray binaries, the recombination time scales for ions such as C IV, Si IV, and N V in the stellar winds of their massive OB companion stars can be very short compared to typical X-ray pulsation or fluctuation time scales. Thus, the authors predict that the 'bleached zones', in which these ions are removed from the stellar wind by X-ray photoionization, will track the X-ray beam as it rotates and that the P Cygni line profiles due to these ions will pulsate. With the IUE satellite the authors obtained low-resolution UV spectra of the binary X-ray system HD 77581/4U 0900-40 resolved into six phase bins of the 283 s pulse period; the observed upper limit to the pulse amplitude of the equivalent width of C IV 1550 A was less than the predicted value. However, the pulsations should be easy to observe with the Hubble Space Telescope.

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