Near-Chandrasekhar-Mass Type Ia Supernovae from the Double-Degenerate Channel

TL;DR

This paper proposes that white dwarf mergers near the Chandrasekhar mass can produce Type Ia supernovae with characteristics similar to the single-degenerate channel, but with distinct delay times and no companion signatures.

Contribution

It introduces a model where WD mergers near M_Ch lead to SNe Ia and Iax, explaining their properties and delay time distribution.

Findings

WD mergers produce highly-magnetized, near-M_Ch WDs.

Near-M_Ch WD mergers can trigger SNe Ia or Iax via rapid spin-up and compression.

Predicted SNe Ia and Iax resemble those from the single-degenerate channel but lack companion signatures.

Abstract

Recent observational evidence has demonstrated that white dwarf (WD) mergers are a highly efficient mechanism for mass accretion onto WDs in the galaxy. In this paper, we show that WD mergers naturally produce highly-magnetized, uniformly-rotating WDs, including a substantial population within a narrow mass range close to the Chandrasekhar mass ($M_{\rm Ch}$). These near-$M_{\rm Ch}$ WD mergers subsequently undergo rapid spin up and compression on a $\sim 10^2$ yr timescale, either leading to central ignition and a normal SN Ia via the DDT mechanism, or alternatively to a failed detonation and SN Iax through pure deflagration. The resulting SNe Ia and SNe Iax will have spectra, light curves, polarimetry, and nucleosynthetic yields similar to those predicted to arise through the canonical near-$M_{\rm Ch}$ single degenerate (SD) channel, but with a $t^{-1}$ delay time distribution characteristic of the double-degenerate (DD) channel. Furthermore, in contrast to the SD channel, WD merger near-$M_{\rm Ch}$ SNe Ia and SNe Iax will not produce observable companion signatures. We discuss a range of implications of these findings, from SNe Ia explosion mechanisms, to galactic nucleosynthesis of iron peak elements including manganese.