# On the mass of supernova progenitors: the role of the $^{12}$C$+^{12}$C reaction

## TL;DR

This paper refines the mass limits of supernova progenitors by incorporating recent insights into the $^{12}$C+$^{12}$C reaction, impacting our understanding of stellar evolution and supernova origins.

## Contribution

It provides new stellar models for 7-10 solar mass stars and revises the mass bounds for supernova progenitors considering recent nuclear reaction rate improvements.

## Key findings

- Revised upper bound for CO white dwarf progenitors.
- Revised lower bound for type II supernova progenitors.
- Impact of $^{12}$C+$^{12}$C reaction rate on stellar evolution.

## Abstract

A precise knowledge of the masses of supernova progenitors is essential to answer various questions of modern astrophysics, such as those related to the dynamical and chemical evolution of Galaxies. In this paper we revise the upper bound for the mass of the progenitors of CO white dwarfs (\mup) and the lower bound for the mass of the progenitors of normal type II supernovae (\mups). In particular, we present new stellar models with mass between 7 and 10 \msun, discussing their final destiny and the impact of recent improvements in our understanding of the low energy rate of the \c12c12 reaction.