Methods of modeling properties these entities include the Δm15 ['Delta M One Five] method, MLCS, and the Stretch method. A 2010 paper by Kelly et al. showed that the Hubble residuals of these objects are correlated with the masses of their host galaxies. That work was motiva
Methods of modeling properties these entities include the Δm15 ['Delta M One Five] method, MLCS, and the Stretch method. A 2010 paper by Kelly et al. showed that the Hubble residuals of these objects are correlated with the masses of their host galaxies. That work was motivated by a 1993 Phillips paper that found a more pronounced correlation with the' "stretch factors" of these objects' (*) light curves. Those light curves decay at the decay rate of nickel-56. They are classified in part by the presence of a 615 nanometer silicon line in their spectra, which notably lack hydrogen lines, a characteristic caused by their low-mass, post-main sequence progenitors. These objects, ubiquitous in cosmology as standard candles, are often contrasted with the core-collapse variety of the same class of cataclysmic variable stars. For 10 points, name this class of supernova that results from the detonation of a white dwarf that has accreted enough mass to surpass the Chandrasekhar Limit.
Methods of modeling properties these entities include the Δm15
Type Ia Supernovae [prompt on Supernovae before mention; prompt on Type I Supernovae at all points; "Supernova" not needed after mentioned]