Physics
Scientific paper
Mar 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..361..186b&link_type=abstract
Active OB-Stars: Laboratories for Stellar and Circumstellar Physics, ASP Conference Series, Vol. 361, Proceedings of the confere
Physics
Scientific paper
The thermal millimeter and radio continua of OB stars are formed in the stellar wind, at large distances from the surface (from ˜ 10 to ˜ 100R_*). Observations at these wavelengths therefore cover geometrical regions that cannot be studied in any other way. The continuum fluxes at long wavelengths are determined by both the mass-loss rate and by the structure that may be present. By using a range of wavelengths one can detect changes of structure with distance. We found evidence that the amount of structure decreases with distance in the stellar wind. The B0 supergiant ɛ Ori is an especially good example of a star showing this effect.
Non-thermal radio fluxes were previously thought to be another indicator of structure in the stellar wind. The work of tet{VanLoo+al05} has shown, however, that these non-thermal radio emitters are most probably all colliding-wind systems. A preliminary reduction of recent millimeter observations of ζ Pup shows variability on the 19.6-hr period. If confirmed, this indicates that Corotating Interaction Regions are an important component of structure at distances beyond 10{R}_*.
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