Evolutionary tracks of binary neutron star progenitors across cosmic times

TL;DR

This paper investigates the evolutionary pathways of binary neutron star progenitors using population synthesis, identifying key formation scenarios, analyzing their delay time distributions, and exploring how these affect merger rates and cosmic chemical enrichment.

Contribution

It introduces a detailed analysis of three main evolutionary tracks for binary neutron star formation and examines their impact on merger delay times and cosmic merger rate evolution.

Findings

Three dominant evolutionary tracks identified for neutron star binary formation.

Delay time distribution is complex and not a simple power-law.

Accretion-induced collapse may dominate at high redshifts.

Abstract

Recent discoveries of gravitational wave sources have advanced our knowledge about the formation of compact object binaries. At present, many questions about the stellar origins of binary neutron stars remain open. We explore the evolution of binary neutron star progenitors with the population synthesis code COSMIC. We identify three dominant evolutionary tracks to form neutron star binaries that merge within the age of the Universe: a scenario that includes a common envelope phase between the first neutron star and its companion, a scenario with almost equal-mass progenitors that evolve quasi-simultaneously and which features a double-core common envelope, and a scenario involving the accretion-induced collapse of an oxygen-neon white dwarf into a neutron star. We show that the distribution of time delays between stellar formation and binary neutron star merger at a given progenitor metallicity does not follow a power-law, but instead features a complex structure that reflects the progenitor properties and the relative contribution of each evolutionary track. We also explore the evolution of the merger rate density with redshift and show that the scenario involving the accretion-induced collapse could be dominant at high redshifts. These results can have important implications for the study of the chemical enrichment of galaxies in r-process elements produced in kilonovae; and of short gamma-ray bursts offsets in their host galaxies.