2000A&AS..144..317C

Radial-velocity observations of the double-lined spectroscopic binaries HD 195850 and HD 201193 have been carried out at the Observatoire de Haute-Provence with the CORAVEL instrument in order to determine their orbital elements. They are as follows o HD 195850: P=37.94106days; T=2444872.24HJD; ω=111.5°; e=0.185; K₁=34.15km/s; K₂=44.72km/s; V₀=0.75km/s; a₁sini=17.51Gm; a₂sini=22.93Gm; M₁sin³i=1.04M_☉; M₂sin³i=0.79M_☉. o HD 201193: P=22.299540days; T=2448137.004HJD; ω=144.7°; e=0.388; K₁=54.15km/s; K₂=54.77km/s; V₀=-13.01km/s; a₁sini=15.31Gm; a₂sini=15.48Gm; M₁sin³i=1.179M_☉; M₂sin³i=1.165M_☉. For HD 195850, we propose a F5V + G2V model on the basis of both the Hipparcos-measured parallax and the Δm_v value, 1.1mag, deduced from the intensities of the correlation dips. HD 201193, for its part, is formed by two quasi-identical F6V stars. Stromgren photometric indices suggest the following physical parameters: M_v=3.6 ; T_eff=6200K; logg=4.2. Using Schaller et al. (1992A&AS...96..269S) evolutionary tracks for stars of solar metallicity, we estimate M=1.25M_☉ for the mass of each component. This system should be somewhat evolved above the ZAMS, and the possibility of eclipses is, a priori, not excluded; it is likely that the components rotate in synchronism with the orbital motion.