The authors have assembled a sample of 42 W Ursae Majoris binary systems (21 W-type, 21 A-type) whose light curves have all been solved by means of the Wilson & Devinney method. The masses, radii and luminosities have been derived assuming the global physical properties of a system are the same as for an analogous detached one, and therefore without any constraint on the physical parameters of the primary star. The main results of this procedure are: (i) the discovery of a substantial continuity of the physical properties from W-type to A-type, suggesting a scenario in which almost all A-type systems are the evolved counterparts of W-types; (ii) the existence of an inhomogeneous group probably evolved into contact from a detached configuration. This second group has no evolutionary link with the RS CVn-like systems, which seemed at first to be suitable candidates as parent stars. An upper limit for the primary mass of unevolved objects is derived.
General properties of W Ursae Majoris systems / Maceroni, C.; Milano, L.; Russo, G.. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 217:4(1985), pp. 843-866. [10.1093/mnras/217.4.843]
General properties of W Ursae Majoris systems
L. MilanoMembro del Collaboration Group
;G. Russo
Membro del Collaboration Group
1985
Abstract
The authors have assembled a sample of 42 W Ursae Majoris binary systems (21 W-type, 21 A-type) whose light curves have all been solved by means of the Wilson & Devinney method. The masses, radii and luminosities have been derived assuming the global physical properties of a system are the same as for an analogous detached one, and therefore without any constraint on the physical parameters of the primary star. The main results of this procedure are: (i) the discovery of a substantial continuity of the physical properties from W-type to A-type, suggesting a scenario in which almost all A-type systems are the evolved counterparts of W-types; (ii) the existence of an inhomogeneous group probably evolved into contact from a detached configuration. This second group has no evolutionary link with the RS CVn-like systems, which seemed at first to be suitable candidates as parent stars. An upper limit for the primary mass of unevolved objects is derived.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.