Abstract
We present the results of our optical study of the eclipsing polar Gaia23cer. We analyze the orbital brightness variability in high ( \(\langle r\rangle\approx 16.5^{m}\) ) and low ( \(\langle r\rangle\approx 19.2^{m}\) ) states. The system has an orbital period \(P_{\textrm{orb}}=102.0665\pm 0.0015\) min and exhibits deep eclipses with a duration \(\Delta t_{\textrm{ecl}}=401.30\pm 0.81\) s. The spectra have a red cyclotron continuum with the Zeeman H \(\alpha\) absorption triplet forming in a magnetic field with a strength \(B=15.2\pm 1.1\) MG. The source of emission lines has a high radial velocity semi-amplitude ( \(K\approx 450\) km s \({}^{-1}\) ), and its eclipse lags behind the eclipse of the white dwarf. The mass \(M_{1}=0.79\pm 0.03\;M_{\odot}\) and temperature \(T=11\,350\pm 650\) K of the white dwarf have been estimated by modelling the spectral energy distribution. The eclipse duration corresponds to a donor mass \(M_{2}=0.10{-}0.13\;M_{\odot}\) and an orbital inclination \(i=84.3^{\circ}{-}87.0^{\circ}\) . The donor temperature was estimated to be \(T\approx 2900\) K by modelling the elliptical variability and eclipse depth.
