X-RAY EMISSION FROM MASSIVE STARS IN CYG OB2

作者：Rauw G^*; Naze Y; Wright N J; Drake J J; Guarcello M G; Prinja R K; Peck L W; Albacete Colombo J F; Herrero A; Kobulnicky H A; Sciortino S; Vink J S

来源：Astrophysical Journal, The - Supplement Series, 2015, 221(1): 1.

DOI：10.1088/0067-0049/221/1/1

• open clusters and associations: individual (Cyg OB2)
• stars: early-type
• stars: Wolf-Rayet
• X-rays: stars

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 L-X/L-bol = -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 L-X and L-bol. 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 L-X/L-bol = -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.

• 出版日期2015-11