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

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


	Document type :	Scientific congresses and symposiums : Paper published in a book
	Discipline(s) :	Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
	To cite this reference:	http://hdl.handle.net/2268/97154

Title :	Non-thermal radio emission from colliding-wind binaries: modelling Cyg OB2 No. 8A and No. 9
Language :	English
Author, co-author :	Volpi, Delia [Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium,]
	Blomme, Ronny [Royal Observatory of Belgium, Ringlaan 3, B-1180 Brussels, Belgium,]
	De Becker, Michaël [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO)]
	Rauw, Grégor [Institut d'Astrophysique, Université de Liège, Allée du 6 Août, 17, Bât B5c, B-4000 Liège (Sart-Tilman), Belgium]
Publication date :	1-Jul-2011
Main document title :	Active OB stars: structure, evolution, mass loss and critical limits
Alternative title :	[en] Proceedings IAU Symposium no. 272
Editor :	Neiner, Coralie
	Wade, G.
	Meynet, G.
	Peters, G.
Pages :	638-639
On invitation :	No
Audience :	International
Keywords :	[en] plasmas ; radiation mechanisms: nonthermal ; methods: numerical ; binaries: spectroscopic ; stars: early-type ; stars: winds ; outflows
Abstract :	[en] 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.
Permalink :	http://hdl.handle.net/2268/97154
DOI :	10.1017/S1743921311011689
Other URL :	http://adsabs.harvard.edu/abs/2011IAUS..272..638V
Commentary :	http://de.arxiv.org/abs/1012.3403

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