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We present high speed photometry and high resolution spectroscopy of theeclipsing post common envelope binary QS Virginis (QS Vir). Our UVES spectraspan multiple orbits over more than a year and reveal the presence of severallarge prominences passing in front of both the M star and its white dwarfcompanion, allowing us to triangulate their positions. Despite showing smallvariations on a timescale of days, they persist for more than a year and maylast decades. One large prominence extends almost three stellar radii from theM star. Roche tomography reveals that the M star is heavily spotted and thatthese spots are long-lived and in relatively fixed locations, preferentiallyfound on the hemisphere facing the white dwarf. We also determine precisebinary and physical parameters for the system. We find that the 14,220 +/- 350Kwhite dwarf is relatively massive, 0.782 +/- 0.013Ms, and has a radius of0.01068 +/- 0.00007Rs, consistent with evolutionary models. The tidallydistorted M star has a mass of 0.382 +/- 0.006Ms and a radius of 0.381 +/-0.003Rs, also consistent with evolutionary models. We find that the magnesiumabsorption line from the white dwarf is broader than expected. This could bedue to rotation (implying a spin period of only ~700 seconds), or due to a weak(~100kG) magnetic field, we favour the latter interpretation. Since the Mstar's radius is still within its Roche lobe and there is no evidence that itsover-inflated we conclude that QS Vir is most likely a pre-cataclysmic binaryjust about to become semi-detached.

The crowded magnetosphere of the post common envelope binary QS Virginis