The Stellar Wind Structure of the Massive Companions of the Binary X-Ray Pulsars in the Magellanic Clouds

Details The Stellar Wind Structure of the Massive Companions of the Binary X-Ray Pulsars in the Magellanic Clouds The Stellar Wind Structure of the Massive Companions of the Binary X-Ray Pulsars in the Magellanic Clouds

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993phdt........26w&link_type=abstract

Thesis (PH.D.)--MASSACHUSETTS INSTITUTE OF TECHNOLOGY, 1993.Source: Dissertation Abstracts International, Volume: 54-06, Secti

Physics

4

Binary Stars

Scientific paper

Self-consistent circumstellar models of two massive X-ray binary (MXRB) systems, SMC X-1 and LMC X-4, have been constructed to account for data obtained from the satellite X-ray observatory Ginga. The circumstellar models for these two MXRBs, which have ultra-luminous X-ray sources, have three characteristic regions: an X-ray heated region, an X-ray shadowed region, and a boundary region between the two. In the X-ray heated region, no line-driven wind is present due to X-ray ionization, but there are indications of a thermal wind caused by X-ray heating. A normal line -driven wind, characteristic of massive and ultra-luminous early-type stars, is expected in the X-ray shadowed region. In the boundary region, a density enhancement is expected according to simulations carried out with a 3D hydrodynamics code. A fast moving line-driven wind piles up on the slow -moving ionized wind and creates a density enhancement called a "photoionization wake". Coriolis force causes this wake to wrap around the companion star and produce an asymmetric density distribution around it. These models are based on physically plausible assumptions and provide a good account of the Ginga data. (Copies available exclusively from MIT Libraries, Rm. 14-0551, Cambridge, MA 02139-4307. Ph. 617 -253-5668; Fax 617-253-1690.).

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