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Rauw, G.; Naze, Y.; Wright, N. J.; Drake, J. J.; Guarcello, M. G.; Prinja, R. K.; Peck, L. W.; Colombo, J. F. Albacete; Herrero, A.; Kobulnicky, H. A.; Sciortino, S.; Vink, J. S. (2014)
Publisher: IOP Publishing Ltd.
Languages: English
Types: Article
Subjects: Astrophysics - Solar and Stellar Astrophysics, QB, Wolf–Rayet [stars], QC, : Aérospatiale, astronomie & astrophysique [Physique, chimie, mathématiques & sciences de la terre], : Space science, astronomy & astrophysics [Physical, chemical, mathematical & earth Sciences], early-type [stars], stars [X-rays], individual: Cyg OB2 [open clusters and associations]
We report on the analysis of the Chandra-ACIS data of O, B, and WR stars in the young association Cyg OB2. X-ray spectra of 49 O-stars, 54 B-stars, and 3 WR-stars are analyzed and for the brighter sources, the epoch dependence of the X-ray fluxes is investigated. The O-stars in Cyg OB2 follow a well-defined scaling relation between their X-ray and bolometric luminosities: log(Lx/Lbol)=-7.2+/- 0.2. This relation is in excellent agreement with the one previously derived for the Carina OB1 association. Except for the brightest O-star binaries, there is no general X-ray overluminosity due to colliding winds in O-star binaries. Roughly half of the known B-stars in the surveyed field are detected, but they fail to display a clear relationship between Lx and Lbol. Out of the three WR stars in Cyg OB2, probably only WR 144 is itself responsible for the observed level of X-ray emission, at a very low log(Lx/Lbol)=-8.8+/- 0.2. The X-ray emission of the other two WR-stars (WR 145 and 146) is most probably due to their O-type companion along with a moderate contribution from a wind–wind interaction zone. Peer reviewed
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