An X-ray Study of a Massive Star and its Wind

Details An X-ray Study of a Massive Star and its Wind An X-ray Study of a Massive Star and its Wind

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1279..363m&link_type=abstract

DECIPHERING THE ANCIENT UNIVERSE WITH GAMMA-RAY BURSTS. AIP Conference Proceedings, Volume 1279, pp. 363-365 (2010).

Astronomy and Astrophysics

Astronomy

Stellar Mass, Shock Waves, Gamma-Ray Sources (Astronomical), Masses, Planetary Bow Shocks, Interplanetary Shocks, Gamma-Ray

Scientific paper

WR 140 is one of the best known examples of a Wolf-Rayet stars. We executed the Suzaku X-ray observations at four different epochs around periastron passage in Jan. 2009 to understand the W-R stellar wind as well as the wind-wind collision shocks. The column density at periastron is about 30 times higher than that at pre-periastron, which can be explained as self-absorption by the Wolf-Rayet wind. The spectra are dominated by a line and continuum emission from a optically thin-thermal plasma. The strong Ne-K lines are evidence that the thermal plasma is shock-heated W-R wind materials by the interaction with the wind from the companion O star. We present the parameters of the wind, such as a mass-loss rate, which were calculated with the absorption and line emission in the spectra.

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