Sensitivity studies for r-process nucleosynthesis in three astrophysical scenarios

TL;DR

This paper reviews sensitivity studies identifying key nuclear physics data affecting r-process nucleosynthesis in three astrophysical scenarios, aiding in understanding element formation in the universe.

Contribution

It presents recent sensitivity analyses that pinpoint the most influential nuclear data for r-process simulations across different astrophysical environments.

Findings

Identifies critical nuclear data impacting r-process outcomes.

Highlights differences in nuclear sensitivities among scenarios.

Provides guidance for future nuclear physics measurements.

Abstract

In rapid neutron capture, or r-process, nucleosynthesis, heavy elements are built up via a sequence of neutron captures and beta decays that involves thousands of nuclei far from stability. Though we understand the basics of how the r-process proceeds, its astrophysical site is still not conclusively known. The nuclear network simulations we use to test potential astrophysical scenarios require nuclear physics data (masses, beta decay lifetimes, neutron capture rates, fission probabilities) for all of the nuclei on the neutron-rich side of the nuclear chart, from the valley of stability to the neutron drip line. Here we discuss recent sensitivity studies that aim to determine which individual pieces of nuclear data are the most crucial for r-process calculations. We consider three types of astrophysical scenarios: a traditional hot r-process, a cold r-process in which the temperature and density drop rapidly, and a neutron star merger trajectory.