Chandra Resolves The Colliding Stellar Wind Binary WR 147 Into A Double Source

Details Chandra Resolves The Colliding Stellar Wind Binary WR 147 Into A Double Source Chandra Resolves The Colliding Stellar Wind Binary WR 147 Into A Double Source

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.4230z&link_type=abstract

American Astronomical Society, HEAD meeting #11, #42.30; Bulletin of the American Astronomical Society, Vol. 41, p.730

Astronomy and Astrophysics

Astronomy

Scientific paper

The enhanced X-ray emission from WR+O binaries likely originates in colliding stellar wind (CSW) shock resulting from the interaction of the hypersonic winds of their massive components. Thus, CSWs in WR+O binaries are an ideal laboratory for studying the wealth of physical processes related to strong shocks and WR 147 is one of the best examples of such a binary system amongst the Wolf-Rayet stars. It has been spatially resolved in the radio, infrared and optical as the binary components are separated by 0.6-0.64 arcsec. Our deep (300 ksec) X-ray observation with the Chandra HETG resolves WR 147 into a double X-ray source. The southern X-ray component is the WN star of the binary system which is also the source of high energy X-rays. The emission mechanism of such a hard emission is yet unclear and we discuss the various possibilities including the presence of a close companion (a third star in the system). The northern X-ray source is softer than its southern counterpart and its emission likely originates in the CSWs although a contribution from the OB companion in this binary system cannot be excluded. Therefore, we discuss all these findings in the framework of the CSW scenario and the possible impact on the corresponding hydrodynamic models.

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