Relativistic Spin Precession in the Double Pulsar

TL;DR

This paper models the eclipse of pulsar A by pulsar B in the double pulsar system to measure relativistic spin precession, providing a test of general relativity in strong gravity conditions.

Contribution

It introduces a simple geometric model to analyze eclipse morphology and measures relativistic spin precession, confirming predictions of general relativity.

Findings

Measured spin precession rate of 4.77 degrees per year

Result consistent with general relativity within 13% uncertainty

Provides a new test of gravity theories in strong-field regime

Abstract

The double pulsar PSR J0737-3039A/B consists of two neutron stars in a highly relativistic orbit that displays a roughly 30-second eclipse when pulsar A passes behind pulsar B. Describing this eclipse of pulsar A as due to absorption occurring in the magnetosphere of pulsar B, we successfully use a simple geometric model to characterize the observed changing eclipse morphology and to measure the relativistic precession of pulsar B's spin axis around the total orbital angular momentum. This provides a test of general relativity and alternative theories of gravity in the strong-field regime. Our measured relativistic spin precession rate of 4.77 (+0.66,-0.65) degrees per year (68% confidence level) is consistent with that predicted by general relativity within an uncertainty of 13%.