Reference : An Exceptional X-ray View of the Young Open Cluster NGC 6231: What XMM-Newton Has Tau...
Scientific congresses and symposiums : Paper published in a book
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/15985
An Exceptional X-ray View of the Young Open Cluster NGC 6231: What XMM-Newton Has Taught Us
English
Sana, H. [> > > >]
Gosset, Eric mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Rauw, Grégor mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) - Sciences spatiales >]
Vreux, Jean-Marie [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > > ]
1-Jan-2006
The X-ray Universe 2005
604
21
No
No
International
[en] Considered as the core of the Sco OB1 association, the young open cluster NGC 6231 harbours a rich O-type star population. In 2001, the XMM-Newton satellite targeted the cluster for a nominal duration of about 180 ks. Thanks to the detector sensitivity, the EPIC cameras provided an unprecedented X-ray view of NGC 6231, revealing about 600 point-like sources. In this contribution, we review the main results that have been obtained thanks to this unprecedented data set. Concerning the O-type stars, we present the latest developments related to the so-called 'canonical' Lx-Lbol relation. The dispersion around this relation might actually be much smaller than previously thought. In our data set, the sole mechanism that yields a significant deviation from this scheme is wind interaction. It is also the sole mechanism that induces a significant variation of the early-type star X-ray flux. In a second part of this contribution, we probe the properties of the optically faint X-ray sources. Most of them are believed to be low mass pre-main sequence stars. Their analysis provides direct insight into the star formation history of the cluster.
http://hdl.handle.net/2268/15985
http://arxiv.org/abs/astro-ph/0511700
http://adsabs.harvard.edu/abs/2006ESASP.604...21S

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