Using $^{44}$Ti Emission to Differentiate Between Thermonuclear Supernova Progenitors

TL;DR

This paper explores how detecting $^{44}$Ti emissions can distinguish between different progenitor models of Type Ia supernovae, providing a new observational method to identify their origins.

Contribution

It demonstrates that $^{44}$Ti detection can differentiate between double-detonation and double-degenerate supernova progenitor channels, advancing understanding of supernova origins.

Findings

$^{44}$Ti detection can discriminate supernova progenitor models.

Late-time light curves of calcium-rich transients are dominated by $^{44}$Ti.

Predictions made for $^{44}$Ti signatures in supernova remnants.

Abstract

The radiosotope $^{44}$Ti is produced through $\alpha$-rich freezeout and explosive helium burning in type Ia supernovae (SNe Ia). In this paper, we discuss how the detection of $^{44}$Ti, either through late-time light curves of SNe Ia, or directly via gamma rays, can uniquely constrain the origin of SNe Ia. In particular, building upon recent advances in the hydrodynamical simulation of helium-ignited double white dwarf binaries, we demonstrate that the detection of $^{44}$Ti in a nearby SN Ia or in a young galactic supernova remnant (SNR) can discriminate between the double-detonation and double-degenerate channels of sub-Chandrasekhar (sub-$M_{\rm Ch}$) and near-Chandrasekhar (near-$M_{\rm Ch}$) SNe Ia. In addition, we predict that the late-time light curves of calcium-rich transients are entirely dominated by $^{44}$Ti.