Disk-corona interactions in soft spectral states of black hole binaries

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dc.creatorZycki, Piotr T.
dc.date2000-11-06
dc.date.accessioned2026-07-07T06:31:55Z
dc.date.available2026-07-07T06:31:55Z
dc.descriptionRe-analysis of some archival X-ray data of black hole binaries in soft spectral states is presented. Results of detailed spectral fitting, including proper physical description of the X-ray reprocessed component, indicate that in most cases the soft, thermal disk emission cannot be described by a simple multi-color blackbody model. Additional Comptonization of those seed photons provides an acceptable description of the soft component, implying a presence of a warm (kT~1 keV), mildly optically thick (tau~10) phase of accreting plasma. Combined spectral/temporal analysis of GS 1124-68 during 'flip-flop' transitions in Very High State suggests that the optically thick accretion flow can proceed in (at least) two modes giving the same time-integrated behaviour (i.e. energy spectra) but very different timing behaviour.
dc.description4 pages, 4 figures. To be published in `Proceedings of the Third Microquasar Workshop: Granada Workshop on Galactic relativistic jet sources', Eds: A. J. Castro-Tirado, J. Greiner and J. M. Paredes, Astrophysics and Space Science, in press
dc.identifierhttps://arxiv.org/abs/astro-ph/0011116
dc.identifierhttp://arxiv.org/abs/astro-ph/0011116
dc.identifier2001, ApSSS, 276, 169
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/98753
dc.subjectAstrophysics
dc.titleDisk-corona interactions in soft spectral states of black hole binaries
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