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Article overview
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Formation of optical lines in black-hole binaries | | Kinwah Wu
; Roberto Soria
; Helen Johnston
; Richard Hunstead
; | | Date: |
22 Dec 2000 | | Subject: | astro-ph | | Affiliation: | Sydney U./MSSL), Roberto Soria (MSSL), Helen Johnston (Sydney U.) and Richard Hunstead (Sydney U. | | Abstract: | The HI Balmer emission lines of black-hole binaries show double-peaked profiles during the high-soft state and the quiescent state. In the high-soft state the profiles are asymmetric with a stronger red peak, but the profiles are symmetric in the quiescent state. We suggest that in the high-soft state the emission lines originate from the temperature-inversion layer caused by irradiative heating of an optically thick accretion disk. Irradiative heating also causes the formation of a disk wind, which mildly absorbs the blue peak of the lines. The double-peaked lines seen in the quiescent state arise from an optically thin disk. In the absence of a disk wind, the lines are unabsorbed and so the symmetry of the line profiles is preserved. | | Source: | arXiv, astro-ph/0101390 | | Services: | Forum | Review | PDF | Favorites | |
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