Radio Observations of Candidate Magnetic O Stars

Details Radio Observations of Candidate Magnetic O Stars Radio Observations of Candidate Magnetic O Stars

Jun 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aspc..388..221s&link_type=abstract

Mass Loss from Stars and the Evolution of Stellar Clusters ASP Conference Series, Vol. 388, proceedings of the conference held 2

Astronomy and Astrophysics

Astronomy

Scientific paper

A number of O stars are suspected to have (weak) magnetic fields because of the observed cyclical variability in their UV wind-lines. However, direct detections of these magnetic fields with optical spectropolarimetry have proven to be very difficult. We have searched for non-thermal radio emission, which would be a strong indication for the presence of a magnetic field. Of our 5 selected candidate magnetic O stars, 3 are detected: ξ Per, which we find to have a non-thermal spectrum, and λ Cep and α Cam which show a thermal spectrum. We also find that the fluxes are lower than the expected free-free (thermal) contribution of the stellar wind. This is in agreement with recent findings that the mass-loss rates from O stars using Hα are overestimated because of clumping in the inner part of the stellar wind.

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