Type Ia supernova sub-classes and progenitor origin

Abstract

This paper presents a short review on the current state of SN Ia progenitor origin. Type Ia supernova explosions (meaning thermonuclear disruption of a white dwarf) are observed to be widely diverse in peak luminosity, lightcurve width and shape, spectral features, and host stellar population environment. In the last decade alone, theoretical simulations and observational data have come together to seriously challenge the long-standing paradigm that all SNe Ia arise from explosions of Chandrasekhar mass white dwarfs. In this review I highlight some of the major developments (and changing views) of our understanding of the nature of SN Ia progenitor systems. I give a brief overview of binary star configurations and their plausible explosion mechanisms, and infer links between some of the various (observationally-categorized) SN Ia sub-classes and their progenitor origins from a theoretical standpoint.

Modelling the chemical evolution of the Milky Way

“…The Chandrasekhar mass in absence of H is M Ch $ 1:44 M and represents the limiting mass for the stability of a C-O WD. In the last years, many variations to these two basic scenarios have been suggested (see Hillebrandt et al 2013;Ruiter 2020 for reviews and Kobayashi et al 2020b), including sub-Chandrasekhar masses for the exploding WD. The alternative scenarios have been proposed to explain the so-called peculiar SNeIa.…”

Common envelope to explosion delay time of Type Ia supernovae

“…There is no consensus neither on the main scenario that brings white dwarfs (WDs) to ignite thermonuclear explosions as type Ia supernovae (SNe Ia), nor on the classification of the different SN Ia scenarios (e.g., Livio & Mazzali 2018;Wang 2018;Jha et al 2019;Ruiz-Lapuente 2019;Soker 2019a;Ruiter 2020 for very recent reviews).…”

Anisotropic Quark Stars with an Interacting Quark Equation of State within the Complexity Factor Formalism

“…Finally, in Figure (5), we show the mass-to-radius relationship for anisotropic stars for both approaches. First we study anisotropies within the vanishing complexity formalism, and we obtain the curve in red.…”