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29 March 2024
 
  » arxiv » astro-ph/0204212

 Article overview


High-Resolution X-ray Imaging of the Colliding Wind Shock in WR147
J.M. Pittard ; I.R. Stevens ; P.M. Williams ; A.M.T. Pollock ; S.L. Skinner ; M.F. Corcoran ; A.F.J. Moffat ;
Date 12 Apr 2002
Subject astro-ph
AffiliationLeeds, UK), I.R. Stevens (Birmingham, UK), P.M. Williams (Ifa Edinburgh, UK), A.M.T. Pollock (Computer & Sci. Co., UK), S.L. Skinner (Colorado, USA), M.F. Corcoran (GSFC, USA), A.F.J. Moffat (Montreal, Canada
AbstractWe analyze new high-resolution Chandra X-ray images of the Wolf-Rayet binary system WR147. This system contains a WN8 star with an early-type companion located 0.6’’ to its north, and is the only known early-type binary with a separation on the sky large enough for the wind-wind collision between the stars to currently be resolved at X-ray energies. The 5 ksec Chandra HRC-I image provides the first direct evidence for spatially extended X-ray emission in an early-type binary system. The X-ray emission peaks close to the position of the radio bow shock and north of the WN8 star. A deeper X-ray image is needed to accurately determine the degree of spatial extension, to exactly align the X-ray and optical/radio frames, and to determine whether part of the detected X-ray emission arises in the individual stellar winds. Simulated X-ray images of the wind-wind collision have a FWHM consistent with the data, and maximum likelihood fits suggest that a deeper observation may also constrain the inclination and wind momentum ratio of this system. However, as the WR wind dominates the colliding wind X-ray emission it appears unlikely that the mass-loss rate and the terminal velocity of the companion wind can be separately determined from X-ray observations. We also note an inconsistency between numerical and analytical estimates of the X-ray luminosity ratio of the stronger and weaker wind components, and conclude that the analytical results are in error.
Source arXiv, astro-ph/0204212
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