X-ray Spectroscopy of Accretion Disks and Stellar Winds in X-Ray Binaries

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dc.creatorLiedahl, Duane A.
dc.creatorWojdowski, Patrick S.
dc.creatorJimenez-Garate, Mario A.
dc.creatorSako, Masao
dc.date2001-05-04
dc.date.accessioned2026-07-07T01:58:22Z
dc.date.available2026-07-07T01:58:22Z
dc.descriptionFrom hot, tenuous gas dominated by Compton processes, to warm, photoionized emission-line regions, to cold, optically thick fluorescing matter, accreting gas flows in X-ray binaries span a huge portion of the parameter space accessible to astrophysical plasmas. The coexistence of such diverse states of material within small volumes (10^33-10^36 cm^3) leaves X-ray spectroscopists with a challenging set of problems, since all such matter produces various X-ray spectral signatures when exposed to hard X rays. Emission-line regions in X-ray binaries are characterized by high radiation energy densities, relatively high particle densities, and velocities ~1000 km/s. In this article, we describe some recent efforts to generate detailed X-ray line spectra from models of X-ray binaries, whose aims are to reproduce spectra acquired with the ASCA, Chandra, and XMM-Newton observatories. With emphasis on the global nature of X-ray line emission in these systems, the article includes separate treatments of high-mass and low-mass systems, as well as summaries of continuum spectroscopy
dc.descriptionto appear in the proceedings of "The Challenge of High Resolution X-ray through Infrared Spectroscopy", Lexington, KY 15-17, 2000, uses newpasp.sty
dc.identifierhttps://arxiv.org/abs/astro-ph/0105084
dc.identifierhttp://arxiv.org/abs/astro-ph/0105084
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/2741
dc.subjectAstrophysics
dc.titleX-ray Spectroscopy of Accretion Disks and Stellar Winds in X-Ray Binaries
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