The Eccentric Binary Millisecond Pulsar in NGC 1851

TL;DR

This paper reports the discovery and detailed timing analysis of a highly eccentric millisecond pulsar in NGC 1851, providing insights into its orbital dynamics and companion characteristics.

Contribution

It presents the first phase-coherent timing solution for PSR J0514-4002A, including relativistic orbital measurements and mass estimates, advancing understanding of eccentric binary MSPs in globular clusters.

Findings

Measured periastron advance rate of 0.01289 degrees/year

Estimated total system mass of 2.453 solar masses

Companion likely a massive white dwarf

Abstract

PSR J0514-4002A is a 5-ms pulsar is located in the globular cluster NGC 1851; it belongs to a highly eccentric (e = 0.888) binary system. It is one of the earliest known examples of a numerous and fast-growing class of eccentric binary MSPs recently discovered in globular clusters. Using the GBT, we have obtained a phase-coherent timing solution for the pulsar, which includes a measurement of the rate of advance of periastron: 0.01289(4) degrees per year, which if due completely to general relativity, implies a total system mass of 2.453(14) solar masses. We also derive m_p < 1.5 solar masses and m_c > 0.96 solar masses. The companion is likely to be a massive white dwarf star.