2010ApJ...719.1767L -
Astrophys. J., 719, 1767-1774 (2010/August-3)
Modeling broadband X-ray absorption of massive star winds.
LEUTENEGGER M.A., COHEN D.H., ZSARGO J., MARTELL E.M., MacARTHUR J.P., OWOCKI S.P., GAGNE M. and HILLIER D.J.
Abstract (from CDS):
We present a method for computing the net transmission of X-rays emitted by shock-heated plasma distributed throughout a partially optically thick stellar wind from a massive star. We find the transmission by an exact integration of the formal solution, assuming that the emitting plasma and absorbing plasma are mixed at a constant mass ratio above some minimum radius, below which there is assumed to be no emission. This model is more realistic than either the slab absorption associated with a corona at the base of the wind or the exospheric approximation that assumes that all observed X-rays are emitted without attenuation from above the radius of optical depth unity. Our model is implemented in XSPEC as a pre-calculated table that can be coupled to a user-defined table of the wavelength-dependent wind opacity. We provide a default wind opacity model that is more representative of real wind opacities than the commonly used neutral interstellar medium (ISM) tabulation. Preliminary modeling of Chandra grating data indicates that the X-ray hardness trend of OB stars with spectral subtype can largely be understood as a wind absorption effect.
Abstract Copyright:
∼
Journal keyword(s):
radiative transfer - stars: early-type - stars: mass-loss - stars: winds, outflows
Simbad objects:
8
Full paper
View the references in ADS
To bookmark this query, right click on this link: simbad:2010ApJ...719.1767L and select 'bookmark this link' or equivalent in the popup menu