Forming Double Neutron Stars using Detailed Binary Evolution Models with POSYDON: Comparison to the Galactic Systems

TL;DR

This study uses detailed binary evolution models with POSYDON to understand the formation of double neutron stars in the Milky Way, revealing a bifurcation in formation channels and constraining key evolutionary parameters.

Contribution

It introduces a bifurcation in the common envelope formation channel for DNSs and constrains core definitions, ejection efficiency, and supernova kick velocities using detailed models.

Findings

Bifurcation explains the split in orbital periods of Galactic DNSs.

Low supernova kick velocities best reproduce observed DNSs.

Merging DNSs originate from progenitors with ~0.2 solar masses of pre-supernova envelope.

Abstract

With over two dozen detections in the Milky Way, double neutron stars (DNSs) provide a unique window into massive binary evolution. We use the POSYDON binary population synthesis code to model DNS populations and compare them to the observed Galactic sample. By tracing their origins to underlying single and binary star physics, we place constraints on the detailed evolutionary stages leading to DNS formation. Our study reveals a bifurcation within the well-known common envelope formation channel for DNSs, which naturally explains an observed split in the orbital periods of the Galactic systems. The two sub-channels are defined by whether the donor star has a helium core (Case B mass transfer) or a carbon-oxygen core (Case C) at the onset of the common envelope, with only the helium core systems eventually merging due to gravitational wave-modulated orbital decay. However, producing DNSs through both sub-channels requires either a generous core definition of $\simeq$ 30% H-fraction or a high common envelope ejection efficiency of $\alpha_{\rm CE}\gtrsim1.2$. By testing different supernova kick velocity models, we find that galactic DNSs are best reproduced using a prescription that favors low velocity kicks ($\lesssim 50 \, \rm km/s$), in agreement with previous studies. Furthermore, our models indicate that merging DNSs are born from a stripped progenitor with a median pre-supernova envelope mass $\sim$ 0.2$M_{\odot}$. Our results highlight the value of detailed evolutionary models for improving our understanding of exotic binary star formation.