Orbital parameters of binary radio pulsars in globular clusters and stellar interactions

TL;DR

This paper explains the distribution of binary radio pulsars in globular clusters using binary-star interaction models, highlighting different formation mechanisms for varying eccentricities.

Contribution

It provides a combined numerical and analytical analysis of how stellar interactions shape pulsar binary eccentricities in clusters.

Findings

High eccentricity binaries likely formed via exchange or merger events.

Intermediate eccentricity systems result from fly-by interactions.

Distribution patterns can be explained by stellar interaction processes.

Abstract

The observed distribution of globular cluster binary radio pulsars in the eccentricity versus orbital period plane can be explained as a result of binary-single star interactions. Our numerical and analytical study hints that the highest eccentricity binaries in clusters are likely to be from exchange and/or merger of a single star with a binary component, while the intermediate eccentricity systems are probably results of fly-by interactions.