X-ray emission from the winds of hot stars

Details X-ray emission from the winds of hot stars X-ray emission from the winds of hot stars

Oct 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...241..300l&link_type=abstract

Astrophysical Journal, Part 1, vol. 241, Oct. 1, 1980, p. 300-305.

Mathematics

Logic

361

Early Stars, Hot Stars, Stellar Winds, X Ray Stars, Emission Spectra, Phenomenology, Radiative Transfer, Stellar Models

Scientific paper

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.

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