Mapping WR140 from infrared spectroscopy and imaging
| dc.creator | Williams, P. M. | |
| dc.creator | Varricatt, W. P. | |
| dc.creator | Marston, A. P. | |
| dc.creator | Ashok, N. M. | |
| dc.date | 2004-11-16 | |
| dc.date.accessioned | 2026-07-25T19:30:53Z | |
| dc.description | Observations of the 1.083-micron He I line in WR140 (HD 193793) show P-Cygni profiles which varied as the binary system went through periastron passage. A sub-peak appeared on the normally flat-topped emission component and then moved across the profile consistent with its formation in the wind-collision region. Variation of the absorption component provided constraints on the opening angle (theta) of the wind-collision region. Infrared (2-10 micron) images observed with a variety of instruments in 2001-04 resolve the dust cloud formed in 2001, and show it to be expanding at a constant rate. Owing to the high eccentricity of the binary orbit, the dust is spread around the orbital plane in a 'splash' and we compare the dust images with the orientation of the orbit. | |
| dc.description | 5 pages, 6 figures, contribution to "Massive Stars in Interacting Binaries", eds. N. St-Louis and A. F. J. Moffat, ASP Conference Series | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0411440 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0411440 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/65457 | |
| dc.subject | Astrophysics | |
| dc.title | Mapping WR140 from infrared spectroscopy and imaging | |
| dc.type | text |