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The double pulsar system PSR J0737-3039A/B is a double neutron star binary,with a 2.4-hour orbital period, which has allowed measurement of relativisticorbital perturbations to high precision. The low mass of the second-formedneutron star, as well as the low system eccentricity and proper motion, pointto a different evolutionary scenario compared to most other known doubleneutron star systems. We describe analysis of the pulse profile shape over 6years of observations, and present the resulting constraints on the systemgeometry. We find the recycled pulsar in this system, PSR J0737-3039A, to be anear-orthogonal rotator, with an average separation between its spin andmagnetic axes of 90 +/- 11 +/- 5 deg. Furthermore, we find a mean 95% upperlimit on the misalignment between its spin and orbital angular momentum axes of3.2 deg, assuming that the observed emission comes from both magnetic poles.This tight constraint lends credence to the idea that the supernova that formedthe second pulsar was relatively symmetric, possibly involving electron-captureonto an O-Ne-Mg core.

The double pulsar: evidence for neutron star formation without an iron core-collapse supernova