All known Type Ia supernova models fail to reproduce the observed luminosity-width correlation

Type Ia supernovae are likely thermonuclear explosions of white-dwarf stars, which are sufficiently dense to allow explosive thermonuclear burning if adequately ignited. However, a robust comparison of theoretical scenarios for the progenitor systems to observations is challenging due to the inability to accurately calculate the dynamics of the explosion and the emitted radiation. We have developed novel observational and numerical methods by exploiting the physical principles behind Type Ia supernovae. The new observational techniques allow the derivation of a specific luminosity-width correlation that does not require radiation transfer calculations for comparison. The new numerical methods allow for the first time to calculate this luminosity-width correlation with a percent accuracy for multidimensional progenitor scenarios with current computational facilities. We show that all known Type Ia supernova models fail to reproduce the observed luminosity-width correlation.