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Modeling broadband X-ray absorption of massive star winds by Leutenegger, Maurice A.; Cohen, David H.; Zsargó, Janos; Martell, Erin M.; MacArthur, James P.; Owocki, Stanley P.; Gagné, Marc; Hillier, D. John is a scholarly article available to read on EtoBox.

What is Modeling broadband X-ray absorption of massive star winds about?

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 \textit{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.

Author

Leutenegger, Maurice A.; Cohen, David H.; Zsargó, Janos; Martell, Erin M.; MacArthur, James P.; Owocki, Stanley P.; Gagné, Marc; Hillier, D. John

Published

2010

Language

EN