Reference : XMM-Newton X-ray study of early type stars in the Carina OB1 association
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/17660
XMM-Newton X-ray study of early type stars in the Carina OB1 association
English
Antokhin, I. I. [> > > >]
Rauw, Grégor mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Vreux, Jean-Marie mailto [Université de Liège - ULg > Département d'astrophysique]
van der Hucht, K. A. [> > > >]
Brown, J. C. [> > > >]
Jan-2008
Astronomy and Astrophysics
Edp Sciences S A
477
2
593-609
Yes (verified by ORBi)
International
0004-6361
Les Ulis Cedex A
[en] stars : early-type ; stars : binaries : general ; X-rays : stars
[en] Aims. X-ray properties of the stellar population in the Carina OB I association are examined with special emphasis on early-type stars. Their spectral characteristics provide some clues to understanding the nature of X-ray formation mechanisms in the winds of single and binary early-type stars. Methods. A timing and spectral analysis of five observations with XMM-Newton is performed using various statistical tests and thermal spectral models. Results. 235 point sources have been detected within the field of view. Several of these sources are probably pre-main sequence stars with characteristic short-term variability. Seven sources are possible background AGNs. Spectral analysis of twenty four sources of type OB and WR 25 was performed. We derived spectral parameters of the sources and their fluxes in three energy bands. Estimating the interstellar absorption for every source and the distance to the nebula, we derived X-ray luminosities of these stars and compared them to their bolometric luminosities. We discuss possible reasons for the fact that, on average, the observed X-ray properties of binary and single early type stars are not very different, and give several possible explanations.
http://hdl.handle.net/2268/17660

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