Quantitative X-ray spectroscopy of massive stars

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dc.creatorOskinova, L. M.
dc.creatorHamann, W. -R.
dc.creatorFeldmeier, A.
dc.date2006-05-22
dc.date.accessioned2026-07-07T07:08:32Z
dc.date.available2026-07-07T07:08:32Z
dc.descriptionRadiative transfer in a clumped winds is used to describe X-ray emission line profiles observed in the XMM-Newton RGS spectrum of the OI star Zeta Puppis. It is shown that this X-ray spectrum can be explained as originating from a multi-temperature collisional plasma located in the wind acceleration zone. The X-rays are attenuated in the clumped stellar wind, which gives characteristic profiles to the emergent lines. We specifically study the N VII emission line in the spectrum of Zeta Pup. Long RGS exposures reveal that the N VII line profile is structured. On the basis of our Zeta Pup atmosphere model, we rule out the presence of N VII in the cool wind component. We suggest that the detailed N VII line structure is due to self-absorption in the hot plasma. Wind clumping also affects the transfer of ionizing radiation in high-mass X-ray binaries (HMXBs). We derive analytical formulae for the ionisation parameter in dependence on the parameters of wind clumping.
dc.description6 pages, 7 figures, in Proc. MSSL Workshop no.2 "High resolution X-ray spectroscopy: towards XEUS and Con-X", MSSL, 27 - 28 March 2006
dc.identifierhttps://arxiv.org/abs/astro-ph/0605560
dc.identifierhttp://arxiv.org/abs/astro-ph/0605560
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/110744
dc.subjectAstrophysics
dc.titleQuantitative X-ray spectroscopy of massive stars
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