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 \sim 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 .