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Table · dataset · 2022

Radial velocities for 3 spectroscopic binaries

Listed in IVOA Registry (Virtual Observatory)

We have obtained high-dispersion spectroscopy and BV photometry of two F-type eclipsing binaries, HD71636 and V1022Cas, plus the A-type system OTAnd.

Description

Transiting Exoplanet Survey Satellite measurements for each system have also been incorporated. The photometry of HD71636 enables a more consistent picture of this 5.01331days, circular-orbit system to emerge.

The F2 V primary has a mass of 1.506{+/-}0.002M{sun} and a radius of 1.583{+/-}0.024R{sun}. The mass of the F5 V secondary is 1.282{+/-}0.002M{sun}, and its radius is 1.314{+/-}0.030R{sun}. Comparison with evolutionary models of the Modules for Experiments in Stellar Astrophysics (MESA) series results in a good fit for a composition of [Fe/H]=0.12 and an age of 0.9Gyr.

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For the F6 V stars of V1022Cas, our analysis produces a period of 12.15616days and an eccentricity of 0.312. The two components have nearly equal masses of 1.626{+/-}0.001M{sun} and 1.607{+/-}0.001M{sun}. The radii of the primary and secondary are 2.570{+/-}0.021R{sun} and 2.445{+/-}0.022R{sun}, respectively.

Comparison with the MESA evolutionary models results in [Fe/H]=0.08 and an age of 1.87Gyr. OTAnd consists of a pair of similar mid-A stars that have an orbital period of 20.85292days and an eccentricity of 0.215. The primary has a mass of 2.253{+/-}0.014M{sun} and a radius of 3.167{+/-}0.013R{sun}.

The corresponding parameters for the secondary are 2.147{+/-}0.011M{sun} and 2.649{+/-}0.015R{sun}, respectively. The MESA series models produce a best fit for this system with [Fe/H]=0.10 and an age of 0.675Gyr. The total apsidal motion in both eccentric systems is less than 1.5{deg}/century.

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