dc.contributor.author |
Nebot Gómez-Morán A. |
|
dc.contributor.author |
Oskinova L. |
|
dc.date.accessioned |
2019-01-22T20:31:41Z |
|
dc.date.available |
2019-01-22T20:31:41Z |
|
dc.date.issued |
2018 |
|
dc.identifier.issn |
0004-6361 |
|
dc.identifier.uri |
https://dspace.kpfu.ru/xmlui/handle/net/147569 |
|
dc.description.abstract |
© ESO 2018. The X-ray emission of O-Type stars was first discovered in the early days of the Einstein satellite. Since then many different surveys have confirmed that the ratio of X-ray to bolometric luminosity in O-Type stars is roughly constant, but there is a paucity of studies that account for detailed information on spectral and wind properties of O-stars. Recently a significant sample of O stars within our Galaxy was spectroscopically identified and presented in the Galactic O-Star Spectroscopic Survey (GOSS). At the same time, a large high-fidelity catalog of X-ray sources detected by the XMM-Newton X-ray telescope was released. Here we present the X-ray catalog of O stars with known spectral types and investigate the dependence of their X-ray properties on spectral type as well as stellar and wind parameters. We find that, among the GOSS sample, 127 O-stars have a unique XMM-Newton source counterpart and a Gaia data release 2 (DR2) association. Terminal velocities are known for a subsample of 35 of these stars. We confirm that the X-ray luminosities of dwarf and giant O stars correlate with their bolometric luminosity. For the subsample of O stars with measure terminal velocities we find that the X-ray luminosities of dwarf and giant O stars also correlate with wind parameters. However, we find that these correlations break down for supergiant stars. Moreover, we show that supergiant stars are systematically harder in X-rays compared to giant and dwarf O-Type stars. We find that the X-ray luminosity depends on spectral type, but seems to be independent of whether the stars are single or in a binary system. Finally, we show that the distribution of log(LX/Lbol) in our sample stars is non-Gaussian, with the peak of the distribution at log(LX/Lbol)≈-6.6. |
|
dc.relation.ispartofseries |
Astronomy and Astrophysics |
|
dc.subject |
Stars: massive |
|
dc.subject |
X-rays: stars |
|
dc.title |
The X-ray catalog of spectroscopically identified Galactic O stars: Investigating the dependence of X-ray luminosity on stellar and wind parameters |
|
dc.type |
Article |
|
dc.relation.ispartofseries-volume |
620 |
|
dc.collection |
Публикации сотрудников КФУ |
|
dc.source.id |
SCOPUS00046361-2018-620-SID85058149224 |
|