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

B. B. P. Perera; C. Kim; M. A. McLaughlin; R. D. Ferdman; M. Kramer; I. H. Stairs; P. C. C. Freire; A. Possenti

doi:10.1088/0004-637X/787/1/51

paper

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

arXiv:1404.1458 · doi:10.1088/0004-637X/787/1/51

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 $3 0^{\circ}$ 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 ( $Δ_{S}$ ) is estimated to be ( $13 8^{\circ} \pm 5^{\circ}$ ) at the current epoch and will likely remain constant until tidal interactions become important in $\sim$ $85$ Myr, at merger.

20 pages, 5 figures, Accepted by ApJ on 1 April 2014

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

Abstract

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