Reference : Investigating the X-ray emission from the massive WR+O binary WR 22 using 3D hydrodyn...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/93744
Investigating the X-ray emission from the massive WR+O binary WR 22 using 3D hydrodynamical models
English
Parkin, E. R. mailto [Institut d'Astrophysique et de Géophysique, Université de Liège, 17 allée du 6 Août, B5c, 4000, Sart Tilman, Belgium; Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Australian National University, Cotter Road, Weston Creek, ACT, 2611, Australia]
Gosset, Eric mailto [Institut d'Astrophysique et de Géophysique, Université de Liège, 17 allée du 6 Août, B5c, 4000, Sart Tilman, Belgium;]
1-Jun-2011
Astronomy and Astrophysics
EDP Sciences
530
119
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] stars: winds ; outflows ; stars: early-type ; stars: individual: WR 22 ; stars: massive ; X-rays: binaries ; hydrodynamics
[en] <BR /> Aims: We examine the dependence of the wind-wind collision and subsequent X-ray emission from the massive WR+O star binary WR 22 on the acceleration of the stellar winds, radiative cooling, and orbital motion. <BR /> Methods: Three dimensional (3D) adaptive-mesh refinement (AMR) simulations are presented that include radiative driving, gravity, optically-thin radiative cooling, and orbital motion. Simulations were performed with instantaneously accelerated and radiatively driven stellar winds. Radiative transfer calculations were performed on the simulation output to generate synthetic X-ray data, which are used to conduct a detailed comparison against observations. <BR /> Results: When instantaneously accelerated stellar winds are adopted in the simulation, a stable wind-wind collision region (WCR) is established at all orbital phases. In contrast, when the stellar winds are radiatively driven, and thus the acceleration regions of the winds are accounted for, the WCR is far more unstable. As the stars approach periastron, the ram pressure of the WR's wind overwhelms the O star's and, following a significant disruption of the shocks by non-linear thin-shell instabilities (NTSIs), the WCR collapses onto the O star. X-ray calculations reveal that when a stable WCR exists the models over-predict the observed X-ray flux by more than two orders of magnitude. The collapse of the WCR onto the O star substantially reduces the discrepancy in the 2-10keV flux to a factor of ≃ 6 at φ = 0.994. However, the observed spectrum is not well matched by the models. <BR /> Conclusions: We conclude that the agreement between the models and observations could be improved by increasing the ratio of the mass-loss rates in favour of the WR star to the extent that a normal wind ram pressure balance does not occur at any orbital phase, potentially leading to a sustained collapse of the WCR onto the O star. Radiative braking may then play a significant rôle for the WCR dynamics and resulting X-ray emission.
Researchers ; Students
http://hdl.handle.net/2268/93744
also: http://hdl.handle.net/2268/91038
10.1051/0004-6361/201016125
http://adsabs.harvard.edu/abs/2011A%26A...530A.119P
http://de.arxiv.org/abs/1104.2383

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