Abstract

CP Pup erupted as a bright, energetic nova in 1942. The photometric and spectroscopic (orbital) periods are both very short (~1.5 Hrs) and slightly different. This is a characteristic of the intermediate polars which contain magnetic white dwarfs or the SU UMa stars. CP Pup is an unusual member of either CV subclass. Even the lowest of previous estimates of the radial velocity amplitude (K) imply a white dwarf mass <0.6 M⊙. This is below the mass limit required by the thermonuclear runaway (TNR) model to produce a nova explosion. We obtained high signal to noise, high resolution (1.2 Å FWHM), blue (3940–4918 Å) spectra using the AAT in an attempt to resolve this discrepancy.KeywordsWhite DwarfMass LimitAstronomical InstituteCataclysmic VariableLine WingThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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