Spectroscopic and photometric study of the new eclipsing polar Gaia23cer

• Published in: arXiv.org
• Main Authors: Kolbin, A I, Pavlenko, E P, V Yu Kochkina, Vinokurov, A S, S Yu Shugarov, Sosnovskij, A A, Antonyuk, K A, Antonyuk, O I, Pit, N V, Suslikov, M V, Galimova, E K, Borisov, N V, Burenkov, A N, Spiridonova, O I
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 23.09.2024
• Subjects: Cyclotrons; Modelling; Orbits; Radial velocity; Spectral energy distribution; White dwarf stars
• ISSN: 2331-8422

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.