Contribution à l'étude des binaires des types F, G, K, M. VIII. HD 195850 et HD 201193, binaires spectroscopiques à raies doubles Contribution to the study of F, G, K, M binaries. VIII. HD 195850 and HD 201193, double-lined spectroscopic binaries

Details Contribution à l'étude des binaires des types F, G, K, M. VIII. HD 195850 et HD 201193, binaires spectroscopiques à raies doubles Contribution to the study of F, G, K, M binaries. VIII. HD 195850 and HD 201193, double-lined spectroscopic binaries Contribution à l'étude des binaires des types F, G, K, M. VIII. HD 195850 et HD 201193, binaires spectroscopiques à raies doubles Contribution to the study of F, G, K, M binaries. VIII. HD 195850 and HD 201193, double-lined spectroscopic binaries

Jun 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000a%26as..144..317c&link_type=abstract

Astronomy and Astrophysics Supplement, v.144, p.317-321

Astronomy and Astrophysics

Astrophysics

1

Stars: Individual: Hd 195850, Hd 201193, Binaries: Spectroscopic, Stars: Fundamental Parameters

Scientific paper

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 = 111o 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 3i = 1.04 M_sun; M_2 sin 3i = 0.79 M_sun. HD 201193: P = 22.299540 days; T = 2448137.004 HJD; omega = 144o 7; e = 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 3i = 1.179 M_sun; M_2 sin 3i = 1.165 M_sun. For HD 195850, we propose a F5V + G2V model on the basis of both the Hipparcos-measured parallax and the Delta m_v 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. Strömgren photometric indices suggest the following physical parameters: M_v = 3.6 ; T_eff = 6200 K; log g = 4.2. Using \cite[Schaller et al. (1992)]{S92} evolutionary tracks for stars of solar metallicity, we estimate M = 1.25 M_sun 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.

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