Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011newa...16..412b&link_type=abstract
New Astronomy, Volume 16, Issue 6, p. 412-419.
Astronomy and Astrophysics
Astronomy
Scientific paper
We present the first analyses of the radial velocity and BV light curves for the eclipsing binary system, V335 Ser. This double-lined eclipsing binary has an eccentricity of 0.14. BV photometric light curves and double-lined radial velocities were solved simultaneously using an improved version of the Wilson-Devinney computer program. The masses and radii of the component stars were obtained as M1 = 2.02 ± 0.01 M&sun;, M2 = 1.84 ± 0.02 M&sun;, R1 = 2.03 ± 0.02 R&sun; and R2 = 1.60 ± 0.01 R&sun;. We estimated the semi-amplitudes of the radial velocity curves of the primary and secondary components as K1 = 106.31 ± 0.88 km s-1 and K2 = 116.94 ± 0.88 km s-1, respectively. As determined by absolute visual magnitude and corrections for interstellar extinction, the distance of the system from earth was found to be d = 219 ± 24 pc. The existence of apsidal motion is presented as means of eclipse time, and the apsidal motion rate was found to be ω=0.01302±0.02563degcycle-1. The corresponding apsidal motion period was found to be U = 261 ± 514 years. Using the absolute properties and apsidal motion parameters obtained from period analysis, we computed the observational and theoretical internal structure constants to be logk2,obs = -1.53 and logk2,theo = -2.44, respectively. We also present the evolutionary status of the component stars in an H-R diagram using solar metallicity and four helium content values. Both component stars are slightly evolved from the ZAMS.
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