Sequence of images showing the expanding shells of gas ejected by the nova V445 Puppis. This system was observed to dramatically increase in brightness in November 2000. Spectroscopic examination of the event revealed the presence of dust around the star, and a surprising lack of hydrogen. These data imply that the star system has erupted before, producing the dust, and that it is most likely formed of a white dwarf star accreting helium from a companion star. The amount of helium builds up on the dwarf s surface until it becomes hot and dense enough to ignite, causing the nova. The system is interesting as it is thought that it may one day become a type 1a supernova, an event widely studied in astrophysics as it can be used to determine distances and for the study of dark energy. Imaged by the NACO adaptive optics on the European Southern Obervatory磗 Very Large Telescope, in Chile.