  We present a photometric and spectroscopic study of HD 50526, an ellipsoidal
binary member of the group Double Periodic Variable stars. Performing
data-mining in photometric surveys and conducting new spectroscopic
observations with several spectrographs during 2008 to 2015, we obtained
orbital and stellar parameters of the system. The radial velocities were
analyzed with the genetic PIKAIA algorithm, whereas Doppler tomography maps for
the H$\alpha$ and H$\beta$ lines were constructed with the Total Variation
Minimization code. An optimized simplex-algorithm was used to solve the
inverse-problem adjusting the light curve with the best stellar parameters for
the system. We find an orbital period of $6.701 \pm 0.001 ~\mathrm{d}$ and a
long photometric cycle of $191 \pm 2 ~\mathrm{d}$. We detected the spectral
features of the coldest star, and modeled it with a $\log{g} = 2.79 \pm 0.02
~\mathrm{dex}$ giant of mass $1.13 \pm 0.02 ~\mathrm{M_{\odot}}$ and effective
temperature $10500 \pm 125 ~\mathrm{K}$. In addition, we determine a mass ratio
$q= 0.206 \pm 0.033$ and that the hot star is a B-type dwarf of mass $5.48 \pm
0.02 ~\mathrm{M_{\odot}}$. The $V$-band orbital light curve can be modeled
including the presence of an accretion disk around the hotter star. This fills
the Roche lobe of the hotter star, and has a radius $14.74 \pm 0.02
~\mathrm{R_{\odot}}$ and temperature at the outer edge $9400 ~\mathrm{K}$. Two
bright spots located in the disk account for the global morphology of the light
curve. The Doppler tomography maps of H$\alpha$ and H$\beta$, reveal complex
structures of mass fluxes in the system.
