X-ray line emission from a fragmented stellar wind

Free access article

Issue		A&A Volume 403, Number 1, May III 2003


Page(s)		217 - 224
Section		Formation and evolution of planetary systems
DOI		http://dx.doi.org/10.1051/0004-6361:20030231

A&A 403, 217-224 (2003)
DOI: 10.1051/0004-6361:20030231

X-ray line emission from a fragmented stellar wind

A. Feldmeier, L. Oskinova and W.-R. Hamann

Astrophysik, Institut für Physik, Universität Potsdam, Am Neuen Palais 10, 14469 Potsdam, Germany
e-mail: lida, wrh@astro.physik.uni-potsdam.de
(Received 29 October 2002 / Accepted 13 February 2003 )

Abstract
We discuss X-ray line formation in dense O star winds. A random distribution of wind shocks is assumed to emit X-rays that are partially absorbed by cooler wind gas. The cool gas resides in highly compressed fragments oriented perpendicular to the radial flow direction. For fully opaque fragments, we find that the blueshifted part of X-ray line profiles remains flat-topped even after severe wind attenuation, whereas the red part shows a steep decline. These box-type, blueshifted profiles resemble recent Chandra observations of the O3 star $\zeta$ Pup. For partially transparent fragments, the emission lines become similar to those from a homogeneous wind.

Key words: stars: winds, outflows -- X-rays: stars -- radiative transfer

Offprint request: A. Feldmeier, afeld@astro.physik.uni-potsdam.de

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