Reference : A first detailed study of the colliding wind WR+O binary WR 30a
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/15966
A first detailed study of the colliding wind WR+O binary WR 30a
English
Gosset, Eric mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Royer, P. [Institut d'Astrophysique et de Géophysique, Université de Liège, Avenue de Cointe, 5, B-4000 Liège, Belgium]
Rauw, Grégor mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Groupe d'astrophysique des hautes énergies (GAPHE) - Sciences spatiales >]
Manfroid, Jean mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO) >]
Vreux, Jean-Marie [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > > ]
1-Oct-2001
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
327
435-451
Yes (verified by ORBi)
International
0035-8711
Oxford
United Kingdom
[en] BINARIES: SPECTROSCOPIC ; STARS: INDIVIDUAL: WR 30A ; STARS: MASS-LOSS ; STARS: WOLF-RAYET
[en] We present a detailed, extensive investigation of the photometric and spectroscopic behaviour of WR 30a. This star is definitely a binary system with a period around 4.6d. We propose the value P=4.619d (sigma=0.002d). The identification of the components as WO4+O5((f)) indicates a massive evolved binary system; the O5 component is a main-sequence or, more likely, a giant star. The radial velocities of the O star yield a circular orbit with an amplitude K[SUB]O[/SUB]=29.9 (sigma=2.1)kms[SUP]-1[/SUP] and a mass function of 0.013 (sigma=0.003)M[SUB]solar[/SUB]. The spectrum of WR 30a exhibits strong profile variations of the broad emission lines that are phase-locked with the orbital period. We report the detection of the orbital motion of the WO component with K[SUB]WO[/SUB]=189kms[SUP]-1[/SUP], but this should be confirmed by further observations. If correct, it implies a mass ratio M[SUB]WO[/SUB] /M[SUB]O[/SUB]=0.16. The star exhibits sinusoidal light variations of amplitude 0.024mag peak-to-peak with the minimum of light occurring slightly after the conjunction with the O star in front. On the basis of the phase-locked profile variations of the Civ lambda4658 blend in the spectrum of the WO, we conclude that a wind-wind collision phenomenon is present in the system. We discuss some possibilities for the geometry of the interaction region.
http://hdl.handle.net/2268/15966
10.1046/j.1365-8711.2001.04755.x
http://adsabs.harvard.edu/abs/2001MNRAS.327..435G

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