Constraints of a pulsation frequency on stellar parameters in the eclipsing spectroscopic binary system: V577 Oph

TL;DR

This study demonstrates how a single pulsation frequency in an eclipsing spectroscopic binary can constrain stellar parameters, including mass, age, and oscillation mode, through spectroscopic and photometric analysis.

Contribution

It provides a method to use pulsation frequency constraints to refine stellar parameters in binary systems, with preliminary spectroscopic analysis of V577 Oph.

Findings

Determined orbital parameters and stellar masses of V577 Oph.

Established a lower age limit of 1 Gyr for the system.

Highlighted the potential of pulsation frequencies to constrain stellar properties.

Abstract

We present a preliminary spectroscopic analysis of the binary system V577Oph, observed during the summer of 2007 on the 2.6m NOT telescope on La Palma. We have obtained time series spectroscopic observations, which show clear binary motion as well as radial velocity variations due to pulsation in the primary star. By modelling the radial velocities we determine a full orbital solution of the system, which yields M_A sin^3 i = 1.562 +/- 0.012 M_solar and M_B sin^3 i = 1.461 +/- 0.020 M_solar. An estimate of inclination from photometry yields a primary mass of 1.6 M_solar. Using this derived mass, and the known pulsation frequency we can impose a lower limit of 1 Gyr on the age of the system, and constrain the parameters of the oscillation mode. We show that with further analysis of the spectra (extracting the atmospheric parameters), tighter constraints could be imposed on the age, metallicity and the mode parameters. This work emphasizes the power that a single pulsation frequency can have for constraining stellar parameters in an eclipsing binary system.