Rediscussion of eclipsing binaries. Paper V. The triple system V455 Aurigae
John Southworth

TL;DR
This paper precisely characterizes the V455 Aurigae triple star system, combining photometric, spectroscopic, and astrometric data to determine the physical properties and orbital configurations of its components.
Contribution
It provides high-precision measurements of the masses, radii, and temperatures of the system's stars, including the first direct detection of the tertiary star's light, and analyzes the system's orbital geometry.
Findings
Eclipsing stars have masses of approximately 1.29 and 1.23 solar masses.
The tertiary star has a mass of about 0.72 solar masses.
The system's outer orbit is inclined at 53 degrees, indicating non-coplanarity.
Abstract
V455 Aur is a detached eclipsing binary containing two F-stars in a 3.15-d orbit with a small eccentricity. Its eclipses were discovered in data from the Hipparcos satellite and a spectroscopic orbit was obtained by Griffin (2001, 2013). Griffin found a long-term variation of the systemic velocity of the eclipsing system due to a third body in a highly eccentric orbit (e = 0.73) with a period of 4200 d. We have used these data, the light curve of V455 Aur from the TESS satellite, and the Gaia EDR3 parallax to determine the physical properties of the components of the system to high precision. We find the eclipsing stars to have masses of 1.289 +/- 0.006 Msun and 1.232 +/- 0.005 Msun, radii of 1.389 +/- 0.011 Rsun and 1.318 +/- 0.014 Rsun and effective temperatures of 6500 +/- 200 and 6400 +/- 200 K. Light from the tertiary component is directly detected for the first time, in the form…
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Taxonomy
TopicsStellar, planetary, and galactic studies · Astronomy and Astrophysical Research · Astro and Planetary Science
