Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...347.1090m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 347, Dec. 15, 1989, p. 1090-1099. Research supported by Lawrence Livermore
Astronomy and Astrophysics
Astronomy
55
Early Stars, Shock Wave Propagation, Stellar Atmospheres, Stellar Winds, X Ray Astronomy, Magnetohydrodynamics, Stellar Models, X Ray Spectra
Scientific paper
A one-dimensional radiation-hydrodynamics code is used to numerically investigate the structure and evolution of shocks in the winds of hot stars. Results are presented for the specific case of Tau Sco, a well-studied main-sequence B star for which there are X-ray data from the Einstien satellite's Solid State Spectrometer. A phenomenological radiative acceleration term and a mass-loss rate consistent with UV observations, are used to determine the time dependence of the temperatures within and X-ray emission from an isolated shock region. The driving acceleration leads to the formation of a two-component shock zone with 'forward' and 'reverse' shocks, each with their own characteristic temperature. A denser cold region forms between the two shocks, which could potentially account for the presence of narrow absorption features that are observed in the UV P Cygni profiles of many hot stars. The X-ray emission spectra from the shocks in the calculations are in good general agreement with two-temperature model fits to Einstein X-ray observations.
Cassinelli Joseph P.
MacFarlane Joseph J.
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