Investigation of the Prompt SNe Ia progenitor nature through the analysis of the chemical composition of globular clusters and circumgalactic clouds

TL;DR

This paper proposes a method to determine the properties of Prompt SNe Ia progenitors by analyzing the chemical composition of globular clusters and circumgalactic clouds, linking supernova nucleosynthesis to observed metallicity patterns.

Contribution

It introduces a novel approach connecting supernova progenitor characteristics with chemical abundances in GCs and CGCs, supported by nucleosynthesis estimates.

Findings

CGCs are formation sites for GCs of both subgroups.

The method aligns with the Single Degenerate Pure Deflagration SNIa model.

Nucleosynthesis estimates support low-mass white dwarf progenitors.

Abstract

A method is proposed for determining the properties of type Ia supernovae from short-lived precursors -- Prompt SNIa. This method is based on the assumption that this subtype of type Ia supernovae exploded into low-metallicity globular clusters (GCs), and is responsible for the enrichment of the high-metallicity subgroup of GCs and circumgalactic clouds (CGCs) with the iron peak elements. We justify that CGCs are the formation places of GCs of both subgroups. The accuracy of the method depends, first, on the number of GCs, the spectra of which have been studied in detail; second, on the number of chemical elements, the abundances of which have been worked out. Only those elements are of interest for this method that are produced in supernova explosions and are not produced at the previous stage of the stellar evolution. Our estimates of nucleosynthesis in low-metallicity supernova GCs are in the best agreement with the following Prompt SNIa model: Single Degenerate Pure Deflagration Models of white dwarfs (WDs) burning with masses in the range from 1.30 Msun to 1.31 Msun if carbon explodes in the centre of a WD with a low central density from 0.5*10^9 g/cm^3 to 10^9 g/cm^3.