Spectroscopic and photometric study of the new eclipsing polar Gaia23cer

TL;DR

This study provides a detailed optical analysis of the new eclipsing polar Gaia23cer, revealing its orbital parameters, magnetic field strength, and component masses through spectroscopic and photometric observations.

Contribution

It presents the first comprehensive spectroscopic and photometric characterization of Gaia23cer, including orbital period, magnetic field, and component masses, which were previously unknown.

Findings

Orbital period of 102.07 minutes with deep eclipses.

Magnetic field strength of approximately 15.2 MG.

White dwarf mass of about 0.79 solar masses.

Abstract

We present the results of the optical study of the new eclipsing polar Gaia23cer. We analyzed the brightness variability of the polar in high ($\langle r \rangle \approx 16.5\mathrm{\,mag}$) and low ($\langle r \rangle \approx 19.2\mathrm{\,mag}$) states. The system has an orbital period $P_{orb} = 102.0665 \pm 0.0015$ min and exhibits deep eclipses with a duration $\Delta t_{ecl} = 401.30 \pm 0.81$ s. The spectra have a red cyclotron continuum with the Zeeman H$\alpha$ absorption triplet forming in a magnetic field with a strength of $15.2 \pm 1.1$ MG. The source of emission lines has a high radial velocity semiamplitude ($K\approx 450$km/s) and its eclipse lags behind the eclipse of the white dwarf. The mass $M_1=0.79 \pm 0.03 M_{\odot}$ and temperature $T=11350 \pm 650 K$ of the white dwarf have been found by modelling the spectral energy distribution. The eclipse duration corresponds to a donor mass $M_2 = 0.10-0.13M_{\odot}$ and an orbital inclination $i=84.3-87.0^{\circ}$. The donor temperature was estimated to be $T\approx 2900K$ by modelling the elliptical variability and eclipse depth.