Relativistic spin precession in the double pulsar
Abstract
The double pulsar PSR J0737-3039A/B consists of two neutron stars in a highly relativistic orbit that displays a roughly 30- second eclipse when pulsar A passes behind pulsar B. Describing this eclipse of pulsar A as due to absorption occurring in the magnetosphere of pulsar B, we successfully used a simple geometric model to characterize the observed changing eclipse morphology and to measure the relativistic precession of pulsar B's spin axis around the total orbital angular momentum. This provides a test of general relativity and alternative theories of gravity in the strong- field regime. Our measured relativistic spin precession rate of 4.77 degrees+(0 degrees.66)(-0 degrees.65) per year ( 68% confidence level) is consistent with that predicted by general relativity within an uncertainty of 13%.
Published in:
Science 321,5885 (2008) 104-107;
Link to original published article:
http://dx.doi.org/10.1126/science.1159295
Keywords
Multidisciplinary Sciences
Date of Version
1-1-2008
Recommended Citation
Breton, R. P.; Kaspi, V. M.; Kramer, M.; McLaughlin, M. A.; Lyutikov, M.; Ransom, S. M.; Stairs, I. H.; Ferdman, R. D.; Camilo, F.; and Possenti, A., "Relativistic spin precession in the double pulsar" (2008). Department of Physics and Astronomy Faculty Publications. Paper 885.
https://docs.lib.purdue.edu/physics_articles/885