X-ray emission from the winds of hot stars
1980; IOP Publishing; Volume: 241; Linguagem: Inglês
10.1086/158342
ISSN1538-4357
Autores Tópico(s)Astrophysics and Star Formation Studies
Resumoview Abstract Citations (489) References (26) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS X-ray emission from the winds of hot stars. Lucy, L. B. ; White, R. L. Abstract A phenomenological theory is proposed for the structure of the unstable line-driven winds of early-type stars. These winds are conjectured to break up into a population of blobs that are being radiatively driven through, and confined by ram pressure of an ambient gas that is not itself being radiatively driven. Radiation from the bow shocks preceding the blobs can account for the X-ray luminosity of zeta Puppis. The theory breaks down when used to model the much lower density wind of tau Scorpii, for then the blobs are destroyed by heat conduction from shocked gas. This effect explains why the profiles of this star's UV resonance lines depart from classical P Cygni form. Publication: The Astrophysical Journal Pub Date: October 1980 DOI: 10.1086/158342 Bibcode: 1980ApJ...241..300L Keywords: Early Stars; Hot Stars; Stellar Winds; X Ray Stars; Emission Spectra; Phenomenology; Radiative Transfer; Stellar Models; Astrophysics; Early-Type Stars:Stellar Winds; Stellar Winds:Models; Stellar Winds:X Rays full text sources ADS | data products SIMBAD (2)
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