SIMBAD references

We report an eclipse-mapping analysis of the 71 s pulsation of DQ Her in the He II λ4686 line. The observed pulse phase-dependent illumination pattern can be explained in terms of an asymmetric oblique dipole accretor model, in which X-ray beams from the accretion poles are reprocessed in two arched accretion curtains and in a vertically extended bright spot (BS) of half-thickness H = (7.4±0.4)x10^–3 R_☉ at the disk rim. The optical pulsation is dominated by reprocessing at the BS, indicating that the 71 s pulsation is the beat period between the white dwarf (WD) spin (P_spin = 70.8 s) and the orbital period. Our results exclude the possibility that the rotation period of the WD is 142 s.