X-Ray Emission from Clump Bow Shocks in Massive Star Wind Flows %C (C) 2007. Southeastern Association for Research in Astronomy. All Rights Reserved.

Details X-Ray Emission from Clump Bow Shocks in Massive Star Wind Flows %C (C) 2007. Southeastern Association for Research in Astronomy. All Rights Reserved. X-Ray Emission from Clump Bow Shocks in Massive Star Wind Flows %C (C) 2007. Southeastern Association for Research in Astronomy. All Rights Reserved.

Sep 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007jsara...1...32b&link_type=abstract

Journal of the Southeastern Association for Research in Astronomy, vol= . 1, p. 32-35

Astronomy and Astrophysics

Astronomy

Stars: Winds, Outflows: Wolf Rayet

Scientific paper

Recent observations have shown that the emission profiles of massive stars such as z Pup and z Ori have unusually hard x-ray emissions, and th= e x-ray line profiles tend to be symmetrical and only slightly blueshifted. We suggest a possible explanation for this: in the highly supersonic stellar winds that form around a massive star, locally denser regions of the wind form axially symmetric bow shock structures. We treat these denser regions as rigid spherical "clumps", and assume that they exist randomly around the star. The bow shock shape is parabolic, with temperatures along the shock in excess of 106 K, decreasing from a maximu= m temperature at the shock head. Taking into account stellar occultation, clump occultation, and optical depth parameters, we simulate the line profiles resulting from emission along the shock. We reasonably reproduce the main features of the observed line profiles, though some parameters, such as the speed of the clumps, remain unclear at this time.

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