Orbital Modulation of Mass Loss in High-Mass X-ray Binaries

Details Orbital Modulation of Mass Loss in High-Mass X-ray Binaries Orbital Modulation of Mass Loss in High-Mass X-ray Binaries

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21343211i&link_type=abstract

American Astronomical Society, AAS Meeting #213, #432.11; Bulletin of the American Astronomical Society, Vol. 41, p.300

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The orbital modulation of stellar wind properties of the primary in high-mass X-ray binary systems, as traced by ultraviolet resonance line profiles, is a result of ionization of the wind by the X-ray source. The far-ultraviolet (FUV) spectral region (900-1200 A) is particularly valuable for studying this phenomenon because of the high ionization lines of O VI 1032-1037 A, P V 1118-1128 A, S IV 1063-1073 A. These lines trace higher ionization states and/or lower (unsaturated) optical depths in the wind than C IV 1550 and Si IV 1400. FUV spectra (velocity resolution 25 km/sec) with good binary orbital phase coverage were obtained for several high-mass X-ray binaries with the Far Ultraviolet Spectroscopic Explorer (FUSE) satellite. In this paper we compare the phase-dependent stellar wind properties of several systems, including V884 Sco (4U1700-37), SMC X-1, LMC X-3, LMC X-4, X Per, and V801 Cen (HD102567) as a function of X-ray luminosity, orbital period, and primary mass.
Based on observations made with the NASA-CNES-CSA Far Ultraviolet Spectroscopic Explorer. This work has been supported in part by NASA grants NNG04GK79G and NNG05GD99G to Catholic University of America.

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