Clark, J. S.; Barnes, A. D. and Charles, P. A.
|DOI (Digital Object Identifier) Link:||http://doi.org/10.1111/j.1365-2966.2007.12047.x|
|Google Scholar:||Look up in Google Scholar|
We present new 8200-8900 Å high-resolution spectroscopic observations of the unusual accreting source SS433. The spectra are highly variable on a night-to-night basis, and are dominated by emission from the Paschen series and O iemission. Differences in line profiles between the two species suggest that they arise in kinematically distinct and highly variable circumstellar regions. Moreover, the strength of O iemission argues against identifying the mass donor as a Wolf-Rayet star since we might expect oxygen to be depleted by the CNO cycle in such a star. Weak N iabsorption lines are present, which, if arising in the photosphere of the mass donor would imply a spectral type of B5 or later. However, no evidence was found for orbital modulation in their radial velocity curves suggesting that they too arise in the accretion-driven outflow. Finally, by analogy to the massive close binary RY Scuti, we suggest that the recent detection of a mid-infrared excess attributed to warm dust may arise in a circumbinary disc, implying that SS433 hosts a rich, highly structured circumstellar environment driven by the high mass-transfer rate from the mass donor.
|Item Type:||Journal Article|
|Keywords:||binaries: close; stars: individual: SS433; stars: individual: V1343 Aquilae; X-rays: binaries|
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Astrid Peterkin|
|Date Deposited:||26 Nov 2008 12:16|
|Last Modified:||14 Jan 2016 17:28|
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