# Neutron Stars in Globular Clusters

**Authors:** Natalia Ivanova, Craig O. Heinke, Frederic A. Rasio  
**arXiv:** [0711.3181](https://arxiv.org/abs/0711.3181)  
**Date:** 2007-11-20  
**Summary page:** https://www.summarizepaper.com/en/paper/0711.3181v1/

## Key points

- Formation of X-ray binaries in dense stellar systems involves dynamical interactions between objects.
- Natalia Ivanova, Craig O. Heinke, and Frederic A. Rasio conducted numerical simulations of 70 globular clusters with varying dynamical properties and a total stellar mass of 2*10^7 Msun.
- Neutron stars (NSs) can be formed via electron-capture supernovae to match observations.
- The simulations explain the observed dependence of the number of low-mass X-ray binaries (LMXBs) on "collision number" as well as the large scatter observed between different globular clusters.
- Good agreement is obtained between models and numbers/characteristics of observed pulsars in Terzan 5 and 47 Tuc for millisecond pulsars.
- Importance of dynamical interactions in understanding formation of X-ray binaries in dense stellar systems is highlighted, along with need to consider alternative mechanisms for NS formation beyond traditional core-collapse supernovae.
- This work contributes to our understanding of how these complex systems evolve over time and provides insights into some extreme astrophysical phenomena.

## Summary

The formation of X-ray binaries in dense stellar systems is a complex process that involves dynamical interactions between objects. In their study, "Neutron Stars in Globular Clusters," Natalia Ivanova, Craig O. Heinke, and Frederic A. Rasio present the results of numerical simulations of 70 globular clusters with varying dynamical properties and a total stellar mass of 2*10^7 Msun. The authors find that to match observations, it is necessary to assume that neutron stars (NSs) can be formed via electron-capture supernovae. The simulations also explain the observed dependence of the number of low-mass X-ray binaries (LMXBs) on "collision number" as well as the large scatter observed between different globular clusters. Furthermore, for millisecond pulsars, the authors obtain good agreement between their models and the numbers and characteristics of observed pulsars in the clusters Terzan 5 and 47 Tuc. This study sheds light on the importance of dynamical interactions in understanding the formation of X-ray binaries in dense stellar systems and highlights the need to consider alternative mechanisms for NS formation beyond traditional core-collapse supernovae. Overall, this work contributes to our understanding of how these complex systems evolve over time and provides insights into some of the most extreme astrophysical phenomena in our universe.