A New Approach to the Supercomputer Simulation of Carbon Burning Sub-grid Physics in Ia Type Supernovae Explosion

Abstract

AbstractSupernovae are the major sources of elements in the periodic table, planets, and life. Type Ia supernovae (SNeIa) are not only sources of elements, but also “standard candles” to measure distances in the Universe. We propose a mechanism of carbon burning that causes non-standard Type Ia supernova explosions. The mechanism is based on intensity variations in the incomplete nuclear burning of carbon. In this case, the explosion energy can vary significantly due to the presence of different regimes of carbon burning during the development of turbulence in the burning zone. The energy released during burning, sufficient for the explosion of a white dwarf (as a type Ia supernova), can be achieved with a smaller Chandrasekhar mass. In addition, the explosion energy of a white dwarf with a Chandrasekhar mass can differ considerably. Such a conclusion can be made from modern observations of incomplete burning and chemistry of burning, which determine the explosion energy. In the present paper, a software tool is proposed to demonstrate a significant difference in the values of the explosion energy obtained with different parameterizations of subgrid carbon burning. For computational experiments, we use a code developed by the authors, which is extended using an adaptive nested grid approach to achieve a more accurate reproduction of turbulent burning.KeywordsComputational AstrophysicsNumerical MethodsHigh-Performance Computing