Abstract
From five-colour photometry of the triple-periodic systems H2252-035 and V1223 Sgr, which have very similar orbital and pulsation periods, we find a significant difference in the wavelength dependence of their short period pulsations. Our results indicate that in H2252-035 this pulse originates in a hot region, probably on the white dwarf (Motch and Pakull, 1981), whereas in V1223 Sgr both pulses are the result of reprocessing of X-rays (in the far side of the accretion disk, and in the companion star, respectively), as suggested by Warner (1985).
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