Rayleigh-Taylor Instabilities in Type Ia Supernova Remnants undergoing Cosmic-Ray Particle Acceleration - Low Adiabatic Index Solutions

TL;DR

This paper explores how cosmic-ray acceleration affects Rayleigh-Taylor instabilities in Type Ia supernova remnants with low adiabatic index gamma, finding minimal impact on mixing and remnant structure.

Contribution

It provides new insights into the effects of low gamma values on R-T instabilities and shows cosmic-ray acceleration does not significantly alter remnant mixing.

Findings

Lower gamma increases shock compression ratio and narrows the inter shock region.

Instability decay leads to limited mixing, independent of gamma for gamma >= 1.2.

Tycho's remnant properties align with gamma=5/3, indicating weak cosmic-ray influence.

Abstract

This study investigates the evolution of Rayleigh-Taylor (R-T) instabilities in Type Ia supernova remnants that are associated with a low adiabatic index gamma, where gamma < 5/3, which reflects the expected change in the supernova shock structure as a result of cosmic-ray particle acceleration. Extreme cases, such as the case with the maximum compression ratio that corresponds to gamma=1.1, are examined. As gamma decreases, the shock compression ratio rises, and an increasingly narrow inter shock region with a more pronounced initial mixture of R-T unstable gas is produced. Consequently, the remnant outline may be perturbed by small-amplitude, small-wavelength bumps. However, as the instability decays over time, the extent of convective mixing in terms of the ratio of the radius of the R-T fingers to the blast wave does not strongly depend on the value of gamma for gamma >= 1.2. As a result of the age of the remnant, the unstable gas cannot extend sufficiently far to form metal-enriched filaments of ejecta material close to the periphery of Tycho's supernova remnant. The consistency of the dynamic properties of Tycho's remnant with the adiabatic model gamma=5/3 reveals that the injection of cosmic rays is too weak to alter the shock structure. Even with very efficient acceleration of cosmic rays at the shock, significantly enhanced mixing is not expected in Type Ia supernova remnants.