Age constraints in the double pulsar system J0737-3039

TL;DR

This paper explores age constraints of the double pulsar system J0737-3039 using spin-down models, revealing formation times that influence neutron star merger rate estimates without affecting other system parameters.

Contribution

It introduces models accounting for relativistic wind effects on pulsar B's spin-down, providing revised formation ages and implications for neutron star coalescence rates.

Findings

Formation of B occurred 80 or 180 Myr ago depending on the model.

Revised ages increase the inferred coalescence rate by up to 40%.

Other parameters like kick velocity and progenitor mass remain unaffected.

Abstract

We investigate the age constraints that can be placed on the double pulsar system using models for the spin-down of the first-born 22.7-ms pulsar A and the 2.77-s pulsar B with characteristic ages of 210 and 50 Myr respectively. Standard models assuming dipolar spin-down of both pulsars suggest that the time since the formation of B is ~50 Myr, i.e. close to B's characteristic age. However, adopting models which account for the impact of A's relativistic wind on B's spin-down we find that the formation of B took place either 80 or 180 Myr ago, depending the interaction mechanism. Formation 80 Myr ago, closer to B's characteristic age, would result in the contribution from J0737-3039 to the inferred coalescence rates for double neutron star binaries increasing by 40%. The 180 Myr age is closer to A's characteristic age and would be consistent with the most recent estimates of the coalescence rate. The new age constraints do not significantly impact recent estimates of the kick velocity, tilt angle between pre and post-supernova orbital planes or pre-supernova mass of B's progenitor.