We present spectrophotometry of the dwarf nova IP Peg during quiescence. The spectra have broad, double peaked emission lines on a blue continuum, characteristic of high-inclination dwarf novae. The emission lines are 96 per cent eclipsed and the orbital hump, which is strong in the continuum, is much weaker in the lines. We introduce a method for the analysis of radial velocities of emission lines which corrects for bias caused by disc asymmetries, and we determine the geometrical and physical parameters of IP Peg. The masses of the white dwarf and red star are MW=1.09±0.10 |M_| and MR = 0.64±0.09 |M_|, and the orbital inclination is i=79.3±0.9°. The secondary star which has a radius RR =0.49±0.03 |R_|, lies near the main sequence mass–radius relation. Our analysis of the eclipse shows good agreement with an accretion disc in Keplerian rotation around the white dwarf. We measured the width of the white dwarf eclipse (|Δφ_ W| = 0.0858±0.001) from the eclipse of the high-velocity emission, and therefore determined the time of mid-eclipse. The radius of the accretion disc during our observations was |≈0.5RL1| (RL1 the inner Lagrangian point distance), and just larger than the radius of total eclipse (0.47 RL1).
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T. R. Marsh (1988) studied this question.
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