V2368 Oph: An eclipsing and double-lined spectroscopic binary used as a photometric comparison star for U Oph

TL;DR

This study reveals that V2368 Oph is an eclipsing, double-lined spectroscopic binary with evolved A-type stars, providing valuable data for testing stellar evolution models.

Contribution

The paper identifies the variable nature of V2368 Oph, determines its orbital parameters, and estimates physical properties, highlighting its importance among evolved A-type eclipsing binaries.

Findings

V2368 Oph is an eclipsing, double-lined spectroscopic binary.

The orbital period is approximately 38.33 days.

Both stars are evolved away from the main sequence.

Abstract

The A-type star HR 6412 = V2368 Oph was used by several investigators as a photometric comparison star for the known eclipsing binary U Oph but was found to be variable by three independent groups, including us. By analysing series of new spectral and photometric observations and a critical compilation of available radial velocities, we were able to find the correct period of light and radial-velocity variations and demonstrate that the object is an eclipsing and double-lined spectroscopic binary moving in a highly eccentric orbit. We derived a linear ephemeris T min.I = HJD (2454294.67 +/- 0.01) + (38.32712 +/- 0.00004)d x E and estimated preliminary basic physical properties of the binary. The dereddened UBV magnitudes and effective temperatures of the primary and secondary, based on our light- and velocity-curve solutions, led to distance estimates that agree with the Hipparcos distance within the errors. We find that the mass ratio must be close to one, but the limited number and wavelength range of our current spectra does not allow a truly precise determination of the binary masses. Nevertheless, our results show convincingly that both binary components are evolved away from the main sequence, which makes this system astrophysically very important. There are only a few similarly evolved A-type stars among known eclipsing binaries. Future systematic observations and careful analyses can provide very stringent tests for the stellar evolutionary theory.