An X-Ray Analysis of α CRU

Details An X-Ray Analysis of α CRU An X-Ray Analysis of α CRU

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010jsara...4...12g&link_type=abstract

Journal of the Southeastern Association for Research in Astronomy, vol. 4, p. 12-14

Astronomy and Astrophysics

Astronomy

X-Rays Stars: Early-Type, Stars: α Cru, Stars: Winds, Outflows

Scientific paper

The star α Cru is an early B type subgiant star recently observed by the Chandra X-ray Observatory. This star is of particular interest due to the observed X-ray emission produced by shocks that form in the stellar wind. We observe hydrogen-like Oviii and helium-like Ovii spectral lines in the Low Energy Transmission Grating spectrum. The Ovii produces a characteristic triplet line. We provide an analysis of the helium-like triplet that explains the conditions in the stellar wind where that line emission is formed. α Cru is also an ultraviolet bright star, so an International Ultraviolet Explorer observation is used to explain the effect of ultraviolet pumping on the forbidden component of the Ovii triplet line. The data appear basically consistent with theoretical models of shocks in stellar winds by Owocki, Castor,& Rybicki (1988) and Feldmeier et al. (1997).

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