1993/02/01 by Paula Szkody, Steve B. Howell
Physics and Astronomy · Engineering · #Stellar, planetary, and galactic studies #Astronomical Observations and Instrumentation #Astronomy and Astrophysical Research
paper · doi:10.1086/172245
We have determined radial velocity solutions for the two eclipsing cataclysmic variables DV UMa and AY Psc, which yield mass estimates for the stellar components. AY Psc appears to have a high mass white dwarf (1.3 solar mass), consistent with its high rate of mass transfer and lack of the hot spot. On the other hand, DV UMa, with its orbital period below the gap, low mass transfer rate, and prominent hot spot modulation, has a low-mass (0.4 solar mass) white dwarf. A low-mass white dwarf is also indicated in the ultrashort period system V503 Cyg. However, the interpretation of V503 Cyg is complicated, since it does not eclipse and the spectroscopic period differs from the period obtained using large-amplitude humps in the continuum light. Possible causes for this difference might be associated with a magnetic nonsynchronously rotating white dwarf, the existence of superhump-type phenomena, or the changing illumination of an irradiated secondary.