Spontaneous Initiation of Detonations in White Dwarf Environments: Determination of Critical Sizes

TL;DR

This study determines the minimum size of hot spots needed to initiate detonations in white dwarf matter, providing key insights for supernova explosion models by exploring various parameters affecting detonation conditions.

Contribution

It offers the first detailed analysis of critical hot spot sizes for detonation initiation in white dwarf environments, considering multiple physical parameters.

Findings

Critical hot spot sizes depend on composition, temperature, and geometry.

Higher background temperatures reduce the size needed for detonation.

The results inform supernova explosion modeling and detonation criteria.

Abstract

Some explosion models for Type Ia supernovae (SN Ia), such as the gravitationally confined detonation (GCD) or the double detonation sub-Chandrasekhar (DDSC) models, rely on the spontaneous initiation of a detonation in the degenerate C/O material of a white dwarf. The length scales pertinent to the initiation of the detonation are notoriously unresolved in multi-dimensional stellar simulations, prompting the use of results of 1D simulations at higher resolution, such as the ones performed for this work, as guidelines for deciding whether or not conditions reached in the higher dimensional full star simulations successfully would lead to the onset of a detonation. Spontaneous initiation relies on the existence of a suitable gradient in self-ignition (induction) times of the fuel, which we set up with a spatially localized non-uniformity of temperature -- a hot spot. We determine the critical (smallest) sizes of such hot spots that still marginally result in a detonation in white dwarf matter by integrating the reactive Euler equations with the hydrodynamics code FLASH. We quantify the dependences of the critical sizes of such hot spots on composition, background temperature, peak temperature, geometry, and functional form of the temperature disturbance, many of which were hitherto largely unexplored in the literature. We discuss the implications of our results in the context of modeling of SNe Ia.