GAIA DR3 2059297390930630400: AN ECCENTRIC BINARY WITH CONSIDERABLE APSIDAL MOTION

Apsidal motion in binary stars refers to the gradual precession of the elliptical orbits of two stars around their common center of mass. This phenomenon occurs due to gravitational interactions, which cause the orientation of the orbit to shift over time. We present the indication of apsidal rotation in the eclipsing binary system Gaia DR3 2059297390930630400 (ZTF J195804.88+343708.1) by using the photometric data from the Zwicky Transient Facility (ZTF) and Transiting Exoplanet Survey Satellite (TESS). We used Peranso to derive the orbital period from ZTF and times of minima from the TESS data.