Realistic Modeling of the Pulse Profile of PSR J0737-3039A

Abstract

The Double Pulsar, PSR J$0737$$-$$3039$A/B, is a unique system in which both neutron stars have been detected as radio pulsars. As shown in Ferdman et al., there is no evidence for pulse profile evolution of the A pulsar, and the geometry of the pulsar was fit well with a double-pole circular radio beam model. Assuming a more realistic polar cap model with a vacuum retarded dipole magnetosphere configuration including special relativistic effects, we create synthesized pulse profiles for A given the best-fit geometry from the simple circular beam model. By fitting synthesized pulse profiles to those observed from pulsar A, we constrain the geometry of the radio beam, namely the half-opening angle and the emission altitude, to be $30^{\circ }$ and $10$ neutron star radii, respectively. Combining the observational constraints of PSR J$0737$$-$$3039$A/B, we are able to construct the full three-dimensional orbital geometry of the Double Pulsar. The relative angle between the spin axes of the two pulsars (${\Delta }_S$) is estimated to be ($138^{\circ }\pm 5^{\circ }$) at the current epoch and will likely remain constant until tidal interactions become important in $\sim$$85$ Myr, at merger.

arXiv comment20 pages, 5 figures, Accepted by ApJ on 1 April 2014

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• Implications of PSR J0737-3039B for the Galactic NS-NS Binary Merger Rate
• A Fan Beam Model for Radio Pulsars. I. Observational Evidence
• Correlated spin-down rates and radio emission in PSR B1859+07
• Toward an Empirical Theory of Pulsar Emission XII: Exploring the Physical Conditions in Millisecond Pulsar Emission Regions
• Multi-frequency study of the peculiar pulsars PSR B0919+06 and PSR B1859+07
• Prospects of constraining the dense matter equation of state from the timing analysis of pulsars in double neutron star binaries: the cases of PSR J0737-3039A and PSR J1757-1854
• A MeerKAT view of the double pulsar eclipses -- Geodetic precession of pulsar B and system geometry