Influences of dynamical disruptions on the evolution of pulsars in globular clusters

TL;DR

This study compares pulsar properties in core-collapsed and non-core-collapsed globular clusters, revealing that dynamical disruptions influence pulsar rotation, luminosity, and binary disruption rates, highlighting the impact of cluster dynamics on pulsar evolution.

Contribution

It provides new evidence that dynamical interactions in globular clusters significantly affect pulsar spin, luminosity, and binary disruption, especially in core-collapsed clusters.

Findings

Pulsars in CCed GCs rotate slower than in Non-CCed GCs.

Radio luminosities at 1.4 GHz are higher in CCed GCs.

Disruption rates and isolated pulsar fractions are higher in CCed GCs.

Abstract

By comparing the physical properties of pulsars hosted by core-collapsed (CCed) and non-core-collapsed (Non-CCed) globular clusters (GCs), we find that pulsars in CCed GCs rotate significantly slower than their counterparts in Non-CCed GCs. Additionally, radio luminosities at 1.4 GHz in CCed GCs are higher. These findings are consistent with the scenario that dynamical interactions in GCs can interrupt angular momentum transfer processes and surface magnetic field decay during the recycling phase. Our results suggest that such effects in CCed GCs are stronger due to more frequent disruptions of compact binaries. This is further supported by the observation that both estimated disruption rates and the fraction of isolated pulsars are predominantly higher in CCed GCs.