The early r-process nucleosynthesis scenarios

TL;DR

This paper compares seven r-process nucleosynthesis scenarios against early Universe observations, concluding that magnetorotational and CEJSN scenarios are most likely responsible for different r-process element peaks.

Contribution

It identifies the most plausible r-process scenarios for early Universe element formation and discusses constraints from observed stellar abundance patterns.

Findings

Magnetorotational r-process likely contributes to elements below the third peak.

CEJSN r-process scenario is favored for the third r-process peak.

Other scenarios like NS-NS mergers and magnetars are less likely major contributors.

Abstract

I compare seven actively studied r-process nucleosynthesis scenarios against observed properties of r-process elements in the early Universe, and conclude that the most likely scenario to contribute to the site of elements below the third r-process peak is the magnetorotational r-process scenario, and that of the third peak is the common envelope jets supernova (CEJSN) r-process scenario. The collapsar and CEJSN r-process scenario might also contribute to the lighter r-process elements, and the binary neutron star (NS-NS) merger r-process scenario might contribute to the third r-process peak. The magnetar, the wind from the newly born NS, and the accretion-induced collapse of a white dwarf r-process scenarios fall short in explaining observations. They might exist, but cannot be major contributors to the r-process in the early Universe. To constrain r-process scenarios in the early Universe, I require that they explain the large scatter in the r-process abundances of very metal-poor stars, account for the correlation between light r-process nucleosynthesis and iron production, and the lack of correlation between the third peak r-process production and iron production, as inferred from very metal-poor stars. I discuss the diversity of the CEJSN r-process scenario and encourage extending its exploration.