Radio emission from WR140

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dc.creatorDougherty, S. M.
dc.creatorBeasley, A. J.
dc.creatorClaussen, M. J.
dc.creatorZauderer, B. A.
dc.creatorBolingbroke, N. J.
dc.date2004-10-07
dc.date.accessioned2026-07-07T02:14:57Z
dc.date.available2026-07-07T02:14:57Z
dc.descriptionMilliarcsecond resolution Very Long Baseline Array (VLBA) observations of the archetype WR+O star colliding-wind binary (CWB) system WR140 have been obtained at 23 epochs between orbital phases 0.74 to 0.97. The emission in the wind-collision region (WCR) is resolved as a bow-shaped arc which rotates as the orbital phase progresses. This rotation provides for the first time the inclination of the orbit (122+/-5 degrees), the longitude of the ascending node (353+/-3 degrees), and the orbit semi-major axis (9.0+/-0.5 mas). The implied distance is 1.85+/-0.16 kpc, which requires the O star to be a supergiant, and leads to a wind-momentum ratio of 0.22. Quasi-simultaneous Very Large Array (VLA) observations show the synchrotron spectra evolve dramatically through the orbital phases observed, exhibiting both optically thin and optically thick emission. The optically thin emission maintains a spectral index of -0.5, as expected from diffusive shock acceleration.
dc.description5 pages, 3 figures (uses asp2004.sty). Contribution to "Massive Stars in Interacting Binaries", Sacacomie, Quebec (Aug 16-20, 2004)
dc.identifierhttps://arxiv.org/abs/astro-ph/0410211
dc.identifierhttp://arxiv.org/abs/astro-ph/0410211
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8336
dc.subjectAstrophysics
dc.titleRadio emission from WR140
dc.typetext

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