Common envelope jets supernova r-process yields can reproduce $\rm [Eu/Fe]$ abundance evolution in the Galaxy

TL;DR

This study demonstrates that common envelope jets supernovae can explain the observed europium to iron ratio evolution in the Milky Way, suggesting they are a significant source of r-process elements.

Contribution

The paper introduces a Galactic chemical evolution model showing CEJSNe as a major contributor to r-process nucleosynthesis, aligning with observed europium abundance trends.

Findings

CEJSNe can reproduce early europium to iron ratios.

CEJSNe contribute significantly to r-process element production.

The model matches observed europium evolution in the Galaxy.

Abstract

We use a numerical Galactic chemical evolution model and find that the common envelope jets supernova (CEJSN) r-process scenario can account for both the very early average ratio of europium to iron and its evolution at later times in the Milky-Way (MW) Galaxy. In the CEJSN scenario a neutron star (NS) spirals-in inside a red supergiant (RSG) star all the way to the core and destroys it. According to this scenario r-process isotopes are nucleosynthesized inside neutron-rich jets that the accretion disk around the NS launches inside the core. The merger of a NS with an RSG core already takes place in the very young Galaxy. We conclude that CEJSNe can be a major contributor to r-process nucleosynthesis.