000002269 001__ 2269
000002269 005__ 20160701171702.0
000002269 037__ $$aASTROimport-426
000002269 100__ $$aBlomme, R.
000002269 245__ $$aRadio observations of massive stars
000002269 260__ $$c2011
000002269 520__ $$aDetectable radio emission occurs during almost all phases of massive star evolution. I will concentrate on the thermal and non-thermal continuum emission from early-type stars. The thermal radio emission is due to free-free interactions in the ionized stellar wind material. Early ideas that this would lead to an easy and straightforward way of measuring the mass-loss rates were thwarted by the presence of clumping in the stellar wind. Multi-wavelength observations provide important constraints on this clumping, but do not allow its full determination. Non-thermal radio emission is associated with binarity. This conclusion was already known for some time for Wolf-Rayet stars and in recent years it has become clear that it is also true for O-type stars. In a massive-star binary, the two stellar winds collide and around the shocks a fraction of the electrons are accelerated to relativistic speeds. Spiralling in the magnetic field these electrons emit synchrotron radiation, which we detect as non-thermal radio emission. The many parameters that influence the resulting non-thermal radio fluxes make the modelling of these systems particularly challenging, but their study will provide interesting new insight into massive stars. 
000002269 773__ $$c67-80$$pBulletin de la Societe Royale des Sciences de Liege$$v80$$y2011
000002269 85642 $$ahttp://esoads.eso.org/abs/2011BSRSL..80...67B
000002269 905__ $$apublished in
000002269 980__ $$aREFERD