Based on optical and infrared survey data spanning $\approx 20$ years of observations, the long-term variability of the polar V379 Vir with a brown dwarf secondary has been studied. By modeling the spectral energy distribution, we constrain the white dwarf's mass to $M_1 = 0.61 \pm 0.05~M_{ \odot}$ and its effective temperature to $T_{ eff} = 10930 \pm 350~K$. Near-infrared photometry yields a donor radius of $R_2 = 0.095 \pm 0.018 R_{ \odot}$ and temperature $T_{ eff} = 1600 \pm 180 K$. Modeling of the cyclotron emission from the accretion spot, detected with the Spitzer infrared telescope, gives an accretion rate of $\dot{ M} \approx 3 \times 10^{ -13} M_{ \odot}/yr$. This rate is consistent with polars in a low accretion state, but significantly higher than expected from wind-driven mass transfer.
Categories: astro-ph.SR astro-ph.HE