We report the discovery of a relatively bright eclipsing binary system , which consists of a white dwarf and a main sequence K7 star with clear signs of chromospheric and spot activity .
The light curve of this system shows \sim 0.2 mag ellipsoidal variability with a period of 0.297549 d and a short total eclipse of the white dwarf .
Based on our analysis of the spectral and photometric data , we estimated the parameters of the system .
The K7V star is tidally deformed but does not fill its Roche lobe ( the filling factor is about 0.86 ) .
The orbital inclination is i = 73 ^ { \circ } .1 \pm 0 ^ { \circ } .2 , the mass ratio is q = M _ { 2 } / M _ { 1 } \approx 0.88 .
The parameters of the K7V star are M _ { 2 } \approx 0.64 M _ { \odot } , R _ { 2 } = 0.645 \pm 0.012 R _ { \odot } , T _ { 2 } \approx 4070 K. The parameters of the white dwarf are M _ { 1 } \approx 0.72 M _ { \odot } , R _ { 1 } = 0.013 \pm 0.003 R _ { \odot } , T _ { 1 } = 8700 \pm 1100 K. Photometric observations in different bands revealed that the maximum depth of the eclipse is in the SDSS r filter , which is unusual for a system of a white dwarf and a late main sequence star .
We suspect that this system is a product of the evolution of a common envelope binary star , and that the white dwarf accretes the stellar wind from the secondary star ( the so-called low-accretion rate polar , LARP ) .