Contribution to the study of F, G, K, M binaries. VIII. HD 195850 and HD 201193, double-lined spectroscopic binaries

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 . . HD 195850: P = 37.94106 days; T = 2444872.24 HJD; omega = 111 degrees 5; e = 0.185; K-1 = 34.15 km s(-1); K-2 = 44.72 km s(-1); V-0 = 0.75 Km s(-1); a(1) sin i = 17.51 Gm; a(2) sin i = 22.93 Gm; M-1 sin(3) i = 1.04 M-circle dot; M(2)sin(3) i = 0.79 M-circle dot . . HD 201193: P = 22.299540 days; T = 2448137.004 HJD; omega = 144 degrees 7; is an element of = 0.388; K-1 = 54.15 km s(-1); K-2 = 54.77 km s(-1); V-0 = -13.01 km s(-1); a(1) sin i = 15.31 Gm; a(2) sin i = 15.48 Gm: M-1 sin(3) i = 1.179 M-circle dot; M-2 sin(3) i = 1.165 M-circle dot. For HD 195850, we propose a F5V + G2V model on the basis of both the Hipparcos-measured parallax and the am,, value, 1.1 mag, 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 = 6200 K; log g = 4.2. Using Schaller et al. (1992) evolutionary tracks for stars of solar metallicity, we estimate M = 1.25 M-circle dot for the mass of each component. This system should be somewhat evolved above the ZAMS, anti the possibility of eclipses is, a priori, not excluded; it is likely that the components rotate in synchronism with the orbital motion.