X-ray emission from the winds of hot stars

摘要: The kinematic model adopted in Paper I for the limiting amplitude state attained by unstable line-driven winds of early-type stars is modified, a crucial but neglected physical effect crudely taken into account, and resulting x-ray spectra compared with observation. In this revised phenomenonlogical theory, radiatively driven shocks are conjectured to result from amplification waves survive until shadowing following compels their decay. consequence shock destruction mechanism, theory predicts that emission continues far out nearly terminal flow; effects self-absorption-in particular, discontinuities at K-shell edges: therefore not now expected be prominent, qualitatively consistent recent analyses Einstein data. Nevertheless, preferred choice theory's single free parameter luminosities calculated several O too low soft. These failures interpreted as implying broad spectrum strengths, bulk coming strongest shocks.