Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...464..434c&link_type=abstract
Astrophysical Journal v.464, p.434
Astronomy and Astrophysics
Astronomy
19
Stars: Binaries: Eclipsing, Shock Waves, Stars: Individual Constellation Name: V444 Cygni, Stars: Mass Loss, X-Rays: Stars
Scientific paper
Phase-resolved ROSA T observations of the soft X-ray flux from the W-R + 0 star binary V444 Cyg confirm the orbital dependence of the flux suggested by Einstein IPC observations, showing a drop in flux around primary eclipse, when the W-R star is in front of the 0 star. The observed X-ray variability can be modeled as a wind eclipse of an X-ray source by the Wolf-Rayet wind. If most of the X-rays from the system are produced in a region of shock-heated gas formed by the wind collision between the two stars, then the shocked gas has a large physical extent (r ˜ l4ORWR) if the observed variability is produced solely by the eclipse of the region by the W-R wind. However, since the 0 star makes a significant contribution to the total X-ray flux from the system, the actual size of the shocked interaction region is probably much smaller. We discuss possible origins for the X-ray emission and conclude that it is probable that at least a fraction of the observed X-ray emission comes from the wind collision.
Corcoran Michael F.
Pollock Andy M. T.
Rawley Gayle L.
Shore Steve N.
Stevens Ian R.
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