Direct and sequential four-body recombination rates at low temperatures

TL;DR

This paper develops a formalism to calculate four-body nuclear recombination rates in stellar environments, showing that these processes dominate over radiative captures at low temperatures and high densities, with implications for stellar nucleosynthesis.

Contribution

The paper introduces a detailed formalism for direct and sequential four-body nuclear recombination reactions, including parameterized cross sections for astrophysical applications.

Findings

Direct four-body reactions dominate at low temperatures.

Sequential mechanisms become comparable at higher temperatures.

Four-body recombination surpasses radiative three-body capture at high densities.

Abstract

We investigate four-body nuclear reactions in stellar environments contributing to creation of light nuclei, exemplified by $^9$Be and $^{12}$C. The originally assumed process is radiative capture, where nuclear clusters combine into the excited final nucleus and photon emission populates the stable nuclear ground states. Instead, we consider nuclear four-body recombination reactions where a spectator nuclear particle replaces the photon. We first develop the elaborate formalism for both, direct and sequential capture processes, where the decaying three-body resonance is formed without and with population of an intermediate two-body resonance, respectively. To facilitate both calculations and practical applications we parameterize the involved cross sections as done successfully in previous computations of reaction rates. We consider the lowest-lying nuclear states with their dominant contributions at low stellar temperatures. We calculate and compare reaction and production rates for different processes. The direct reaction mechanism dominates by many orders of magnitude at low temperature, where the sequential stepping stones are energetically too expensive to use. At somewhat higher temperatures these two different nuclear four-body mechanisms become comparable. Comparison to radiative three-body capture reveals already formally, but also numerically, that four-body nuclear recombination must dominate for sufficiently high nuclear densities. Numerical values are given for all these rates as function of temperature and density. The relative importance is exhibited.