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| Nature 428, 919 - 921 (29 April 2004); doi:10.1038/nature02509 The geometry of the double-pulsar system J0737–3039 from systematic intensity variations FREDRICK A. JENET1 AND SCOTT M. RANSOM2,3 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109, USA 2 Physics Department, McGill University, 3600 University Street, Montreal, Quebec H3A 2T8, Canada 3 Center for Space Research, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA Correspondence and requests for materials should be addressed to F.J. (merlyn@alum.mit.edu). Two pulsars (PSR J0737–3039A and B) were recently discovered in highly relativistic orbits around one another. 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, referred to here 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 its orbit. Here we report a geometrical model of the system that simultaneously explains the intensity variations of B and provides constraints on the spin axis orientation and emission geometry of A. Our model assumes that B's pulsed radio flux increases when illuminated by emission from A. We predict that A's pulse profile will evolve considerably over the next several years owing to geodetic precession until it disappears entirely in 15–20 years. © 2004 Nature Publishing Group Privacy Policy |
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