Reference : The mass of the very massive binary WR21a
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/200958
The mass of the very massive binary WR21a
English
Tramper, F. [University of Amsterdam > Anton Pannenkoek Institute for Astronomy > > >]
Sana, H. [Katholieke Universiteit Leuven - KUL > Instituut of Sterrenkunde > > >]
Fitzsimons, N. E. [University of Amsterdam > Anton Pannenkoek Institute for Astronomy > > >]
de Koter, A. [University of Amsterdam > Anton Pannenkoek Institute for Astronomy > > >]
Kaper, L. [University of Amsterdam > Anton Pannenkoek Institute for Astronomy > > >]
Mahy, Laurent mailto [Université de Liège > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Moffat, A. [Université de Montréal - UdeM > Département de Physique > > >]
2016
Monthly Notices of the Royal Astronomical Society
Blackwell Publishing
Yes (verified by ORBi)
International
0035-8711
1365-2966
Oxford
United Kingdom
[en] binaries: close ; binaries: spectroscopic ; stars: early-type ; stars:fundamental parameters ; stars: individual: WR21a ; stars: Wolf-Rayet
[en] We present multi-epoch spectroscopic observations of the massive binary system WR21a,
which include the 2011 January periastron passage. Our spectra reveal multiple SB2 lines and
facilitate an accurate determination of the orbit and the spectral types of the components. We
obtain minimum masses of 64.4±4.8 Msun and 36.3±1.7 Msun for the two components of
WR21a. Using disentangled spectra of the individual components, we derive spectral types of
O3/WN5ha and O3Vz ((f*)) for the primary and secondary, respectively. Using the spectral
type of the secondary as an indication for its mass, we estimate an orbital inclination of i=58.8±2.5° and absolute masses of 103.6±10.2 Msun and 58.3±3.7 Msun, in agreement with the luminosity of the system. The spectral types of the WR21a components indicate that the stars are very young (1–2 Myr), similar to the age of the nearby Westerlund 2 cluster. We use evolutionary tracks to determine the mass–luminosity relation for the total system mass. We find that for a distance of 8 kpc and an age of 1.5 Myr, the derived absolute masses are in good agreement with those from evolutionary predictions.
Liège Space Research Institute - LiSRI
Fonds de la Recherche Scientifique (Communauté française de Belgique) - F.R.S.-FNRS ; Action de Recherche Concertée, ARC, Etoiles massives
Researchers ; Students
http://hdl.handle.net/2268/200958
10.1093/mnras/stv2373
http://adsabs.harvard.edu/abs/2016MNRAS.455.1275T

File(s) associated to this reference

Fulltext file(s):

FileCommentaryVersionSizeAccess
Open access
MNRAS-2016-Tramper-1275-81.pdfPublisher postprint407.02 kBView/Open

Bookmark and Share SFX Query

All documents in ORBi are protected by a user license.