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Non-thermal radio emission from colliding-wind binaries: modelling Cyg OB2 No. 8A and No. 9

Published online by Cambridge University Press:  12 July 2011

Delia Volpi ,
Ronny Blomme ,
Michael De Becker  and
Gregor Rauw
Delia Volpi
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium, email: delia.volpi@oma.be
Ronny Blomme
Affiliation:
Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium, email: delia.volpi@oma.be
Michael De Becker
Affiliation:
Institut d'Astrophysique, Université de Liège, Allée du 6 Août, 17, Bât B5c, B-4000 Liège (Sart-Tilman), Belgium Observatoire de Haute-Provence, F-04870 Saint-Michel l'Observatoire, France
Gregor Rauw
Affiliation:
Institut d'Astrophysique, Université de Liège, Allée du 6 Août, 17, Bât B5c, B-4000 Liège (Sart-Tilman), Belgium
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Abstract

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Some OB stars show variable non-thermal radio emission. The non-thermal emission is due to synchrotron radiation that is emitted by electrons accelerated to high energies. The electron acceleration occurs at strong shocks created by the collision of radiatively-driven stellar winds in binary systems. Here we present results of our modelling of two colliding wind systems: Cyg OB2 No. 8A and Cyg OB2 No. 9.

Keywords

plasmasradiation mechanisms: nonthermalmethods: numericalbinaries: spectroscopicstars: early-typestars: windsoutflows

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