Reference : MULTIWAVELENGTH OBSERVATIONS OF THE RUNAWAY BINARY HD 15137
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/24348
MULTIWAVELENGTH OBSERVATIONS OF THE RUNAWAY BINARY HD 15137
English
McSwain, M. V. [ > > ]
De Becker, Michaël mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO) >]
Roberts, M. S. E. [ > > ]
Boyajian, T. S. [ > > ]
Gies, D. R. [ > > ]
Grundstrom, E. D. [ > > ]
Aragona, C. [ > > ]
Marsh, A. N. [ > > ]
Roettenbacher, R. M. [ > > ]
Mar-2010
Astronomical Journal (The)
Univ Chicago Press
139
857
Yes
International
0004-6256
Chicago
IL
[en] stars: early-type ; Spectroscopic binaries ; accretion and accretion disks ; neutron stars ; black holes ; stars : HD15137 ; X-rays: stars
[en] HD 15137 is an intriguing runaway O-type binary system that offers a rare opportunity to explore the mechanism by which it was ejected from the open cluster of its birth. Here, we present recent blue optical spectra of HD 15137 and derive a new orbital solution for the spectroscopic binary and physical parameters of the O star primary. We also present the first XMM-Newton observations of the system. Fits of the EPIC spectra indicate soft, thermal X-ray emission consistent with an isolated O star. Upper limits on the undetected hard X-ray emission place limits on the emission from a proposed compact companion in the system, and we rule out a quiescent neutron star (NS) in the propeller regime or a weakly accreting NS. An unevolved secondary companion is also not detected in our optical spectra of the binary, and it is difficult to conclude that a gravitational interaction could have ejected this runaway binary with a low mass optical star. HD 15137 may contain an elusive NS in the ejector regime or a quiescent black hole with conditions unfavorable for accretion at the time of our observations.
Researchers ; Professionals
http://hdl.handle.net/2268/24348
10.1088/0004-6256/139/3/857
http://iopscience.iop.org/1538-3881/139/3/857/

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