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 cha
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]