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V445 Pup was a peculiar nova with no hydrogen spectral lines during theoutburst. The spectrum contained strong emission lines of carbon, oxygen,calcium, sodium, and iron. We have performed digital processing of photographicimages of the V445 Pup progenitor using astronomical plate archives. Thebrightness of the progenitor in the B band was 14.3 mag. It was a periodicvariable star, its most probable period being 0.650654+/-0.000011 day. Thelight curve shape suggests that the progenitor was a common-envelope binarywith a spot on the surface and variable surface brightness. The spectral energydistribution of the progenitor between 0.44 and 2.2 micrometers was similar tothat of an A0V type star. After the explosion in 2001, the dust was formed inthe ejecta, and the star became a strong infrared source. This resulted in thestar's fading below 20 mag in the V band. Our CCD BVR observations acquiredbetween 2003 and 2009 suggest that the dust absorption minimum finished in2004, and the remnant reappeared at the level of 18.5 mag V. The dust dispersedbut a star-like object was absent in frames taken in the K band with the VLTadaptive optics. Only expanding ejecta of the explosion were seen in theseframes till March 2007. No reddened A0V type star reappeared in the spectralenergy distribution. The explosion of V445 Pup in 2000 was a helium flash onthe surface of a CO-type white dwarf. Taking into account the results of moderndynamic calculations, we discuss the possibility of a white-dwarf coredetonation triggered by the helium flash and the observational evidence for it.Additionally, the common envelope of the system was lost in the explosion.Destruction in the system and mass loss from its components exclude the futureSN Ia scenario for V445 Pup.

The progenitor and remnant of the helium nova V445 Puppis