X-ray Spectroscopy of the Contact Binary VW Cephei
| dc.creator | Huenemoerder, David P. | |
| dc.creator | Testa, Paola | |
| dc.creator | Buzasi, Derek L. | |
| dc.date | 2006-06-28 | |
| dc.date.accessioned | 2026-07-07T10:39:25Z | |
| dc.date.available | 2026-07-07T10:39:25Z | |
| dc.description | Short-period binaries represent extreme cases in the generation of stellar coronae via a rotational dynamo. Such stars are important for probing the origin and nature of coronae in the regimes of rapid rotation and activity saturation. VW Cep (P=0.28 d) is a relatively bright, partially eclipsing, and very active object. Light curves made from Chandra/HETGS data show flaring and rotational modulation, but no eclipses. Velocity modulation of emission lines indicates that one component dominates the X-ray emission. The emission measure is highly structured, having three peaks. Helium-like triplet lines give electron densities of about 3.0E+10 - 18.0E+10 /cm^3. We conclude that the corona is predominantly on the polar regions of the primary star and compact. | |
| dc.description | Accepted for publication in the Astropysical Journal, 23 June 2006; 22 pages, 15 figures | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0606690 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0606690 | |
| dc.identifier | Astrophys.J.650:1119-1132,2006 | |
| dc.identifier | doi:10.1086/507404 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/181024 | |
| dc.subject | Astrophysics | |
| dc.title | X-ray Spectroscopy of the Contact Binary VW Cephei | |
| dc.type | text |