{ "id": "astro-ph/0111134", "version": "v2", "published": "2001-11-07T01:48:12.000Z", "updated": "2002-01-14T00:23:19.000Z", "title": "The X-ray Spectra of Black Hole X-ray Novae in Quiescence as Measured by Chandra", "authors": [ "A. K. H. Kong", "J. E. McClintock", "M. R. Garcia", "S. S. Murray", "D. Barret" ], "comment": "9 pages, 6 figures, accepted for publication in ApJ", "doi": "10.1086/339501", "categories": [ "astro-ph" ], "abstract": "We present Chandra observations of black hole X-ray novae V404 Cyg, A0620-00, GRO J1655-40 and XTE J1550-564 in quiescence. Their quiescent spectra can be well fitted by a power-law model with slope $\\alpha \\sim 2$. While a coronal (Raymond-Smith) model is also a statistically acceptable representation of the spectra, the best fit temperatures of these models is $\\sim 5$ times higher than that seen in active stellar coronae. These four spectra of quiescent X-ray novae are all consistent with that expected for accretion via an advection-dominated accretion flow (ADAF) and inconsistent with that expected from a stellar corona. This evidence for continued accretion in quiescence further strengthens the case for the existence of event horizons in black holes. Both A0620-00 and GRO J1655-40 were fainter than in previous observations, while V404 Cyg was more luminous and varied by a factor of 2 in a few ksec. A reanalysis of the X-ray data for XTE J1550-564 shows that (like V404 Cyg and A0620-00) its luminosity exceeds the maximum prediction of the coronal model by a large factor. The 0.3-7 keV luminosity of the four sources studied ranges from $\\sim 10^{30}-10^{33}$ erg/s.", "revisions": [ { "version": "v2", "updated": "2002-01-14T00:23:19.000Z" } ], "analyses": { "keywords": [ "x-ray spectra", "quiescence", "hole x-ray novae v404 cyg", "black hole x-ray novae v404" ], "tags": [ "journal article" ], "note": { "typesetting": "TeX", "pages": 9, "language": "en", "license": "arXiv", "status": "editable" } } }