Testing Shock Theories of X-Ray Emission in the Young Nearby O-Star Sigma Orionis

Details Testing Shock Theories of X-Ray Emission in the Young Nearby O-Star Sigma Orionis Testing Shock Theories of X-Ray Emission in the Young Nearby O-Star Sigma Orionis

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002cxo..prop.1133s&link_type=abstract

Chandra Proposal ID #04200261

Physics

Chandra Proposal Id #04200261

Scientific paper

Current theoretical models attribute the X-ray emission of single O-type stars to strong shocks that form in their line-driven winds. Such models predict cool X-ray emission (kT < 1 keV) and blueshifted asymmetric emission lines. In contrast, HETG observations of some O stars show hot dense plasma and broad symmetric lines. These results have sparked renewed interest in hot star X-ray emission models that involve magnetic wind confinement. We propose to observe the young O9V star Sigma Ori with HETG in order to obtain data on line shapes, centroid shifts, and plasma properties needed to determine if its X-ray emission is produced by instability-driven shocks and to guide the development of new models that incorporate dynamic wind-magnetic field interactions.

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