ISSN:
1572-946X
Keywords:
X-rays
;
Winds
;
Hot Stars
Source:
Springer Online Journal Archives 1860-2000
Topics:
Physics
Notes:
Abstract We estimate X-ray emission by shock-heated regions in hot star winds, using temperature and density profiles calculated by time-dependent dynamical models; the shocks result from the instability of the line scattering force that drives the wind. For main sequence late O and early B stars, the model X-ray flux is generally well below the observed flux, though the shape of the model spectrum is approximately consistent with observations. For the early O supergiantζ Pup, the model spectral shape again agrees with observation; the total flux predicted by models is well above the observed flux, though significant uncertainties remain.
Type of Medium:
Electronic Resource
URL:
http://dx.doi.org/10.1007/BF01091172
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