Hynes, R.I. and Haswell, C. A.
|DOI (Digital Object Identifier) Link:||http://dx.doi.org/10.1046/j.1365-8711.1999.02227.x|
|Google Scholar:||Look up in Google Scholar|
We present HST/FOS ultraviolet and optical spectroscopy of the black hole X-ray transient GRO J0422+32 shortly before the system reached quiescence. We find that the accretion spectrum from 2500 to 9000 Å can be very well fitted by a self-absorbed synchrotron model, with superposed H I and Mg II emission lines. The explanations that we suggest for this spectrum are either that it is due to active coronal regions above a geometrically thin accretion disc, or that the disc is evaporated into an advective flow.
|Item Type:||Journal Article|
|Keywords:||accretion, accretion discs – binaries: close – stars: individual: GRO 0422+32 – ultraviolet: stars.|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Astrid Peterkin|
|Date Deposited:||25 Jul 2008 11:18|
|Last Modified:||14 Jan 2016 17:02|
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