Radio emission from WR140

Details Radio emission from WR140 Radio emission from WR140

2004-10-07

arxiv.org/abs/astro-ph/0410211v1

Astronomy and Astrophysics

Astrophysics

5 pages, 3 figures (uses asp2004.sty). Contribution to "Massive Stars in Interacting Binaries", Sacacomie, Quebec (Aug 16-20,

Scientific paper

Milliarcsecond 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.

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