X-ray temperatures and their radial distributions from winds of O-type supergiants: the effects of clumps

Details X-ray temperatures and their radial distributions from winds of O-type supergiants: the effects of clumps X-ray temperatures and their radial distributions from winds of O-type supergiants: the effects of clumps

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010a%26a...512a..50g&link_type=abstract

Astronomy and Astrophysics, Volume 512, id.A50

Astronomy and Astrophysics

Astrophysics

2

Stars: Early Type, Stars: Individual: Ζ Ori A, Stars: Individual: Ζ Pup, Stars: Winds, Outflows, X-Ray: Stars

Scientific paper

Context. Based on the multiphase hydrodynamical flows and the clump model, a two-fluid model of the O stars ζ Ori A and ζ Pup is investigated, in which the flow is described by a set of two components. Aims: I investigate the influence of clumps on the production of X-ray and derive wind parameters from a comparison with the X-ray temperature distributions in the wind of O-type supergiants. Methods: The velocity structure of the clump is assumed to be beta law, thus the transonic velocity structure of the ambient wind can be attained via the shooting method. Results: The mass, filling factor, and velocity structure of the clump are very sensitive to the post-shock temperatures. I find that the filling factor must be about 0.01 for fitting the observed X-ray temperatures. The mass of the clump cannot be smaller than 1018 g. A clump carries about 10-4 dot{M} and 10-5 dot{M} for ζ Ori A and ζ Pup, respectively. The model with the exponent of clump velocity β = 0.5-0.6 for O-type supergiants fits the observations better than one with the exponent β = 0.8. Conclusions: These results indicate that the forward shock scenario can explain the X-ray emission, except for the hottest X-ray lines for O-type supergiants. Theoretical and observable evidence shows that a low velocity law should be applied to O-type supergiants.

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