The geometry of the double-pulsar system J0737-3039 from systematic intensity variations
arXiv:astro-ph/0404569 · doi:10.1038/nature02509
Abstract
The recent discovery of J0737-3039A & B-two pulsars in a highly relativistic orbit around one another - offers an unprecedented opportunity to study the elusive physics of pulsar radio emission. The system contains a rapidly rotating pulsar with a spin period of 22.7 ms and a slow companion with a spin period of 2.77 s, hereafter referred to as 'A' and 'B', respectively. A unique property of the system is that the pulsed radio flux from B increases systematically by almost two orders-of-magnitude during two short portions of each orbit. Here, we describe a geometrical model of the system that simultaneously explains the intensity variations of B and makes definitive and testable predictions for the future evolution of the emission properties of both stars. Our model assumes that B's pulsed radio flux increases when illuminated by emission from A. This model provides constraints on the spin axis orientation and emission geometry of A and predicts that its pulse profile will evolve considerably over the next several years due to geodetic precession until it disappears entirely in 15-20 years.
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- Long-term variations in the pulse emission from PSR J0737-3039B
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- The Mean Pulse Profile of PSR J0737-3039A
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