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A simulation of the thermonuclear explosion of a Chandrasekhar-mass C+O whitedwarf, the most popular scenario of a type Ia supernova (SN Ia), is presented.The underlying modeling is pursued in a self-consistent way, treating thecombustion wave as a turbulent deflagration using well tested methods developedfor laboratory combustion and based on the concept of `large eddy simulations'(LES). Such consistency requires to capture the onset of the turbulent cascadeon resolved scales. This is achieved by computing the dynamical evolution on a1024$^3$ moving grid, which resulted in the best-resolved three-dimensional SNIa simulation carried out thus far, reaching the limits of what can be done onpresent supercomputers. Consequently, the model has no free parameters otherthan the initial conditions at the onset of the explosion, and therefore it hasconsiderable predictive power. Our main objective is to determine to whichextent such a simulation can account for the observations of normal SNe Ia.Guided by previous simulations with less resolution and a less sophisticatedflame model, initial conditions were chosen that yield a reasonably strongexplosion and a sufficient amount of radioactive nickel for a bright display.We show that observables are indeed matched to a reasonable degree. Inparticular, good agreement is found with the light curves of normal SNe Ia.Moreover, the model reproduces the general features of the abundancestratification as inferred from the analysis of spectra. This indicates that itcaptures the main features of the explosion mechanism of SNe Ia. However, wealso show that even a seemingly best-choice pure deflagration model hasshortcomings that indicate the need for a different mode of nuclear burning atlate times, perhaps the transition to a detonation at low density.

A three-dimensional deflagration model for Type Ia supernovae confronted with observations