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arXiv · 0807.2644

Relativistic Spin Precession in the Double Pulsar

Rene P. Breton·Victoria M. Kaspi·Michael Kramer·Maura A. McLaughlin·Maxim Lyutikov·Scott M. Ransom·Ingrid H. Stairs·Robert D. Ferdman·Fernando Camilo·Andrea Possenti
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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 use 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 (+0.66,-0.65) degrees per year (68% confidence level) is consistent with that predicted by general relativity within an uncertainty of 13%.

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Rene P. Breton, Victoria M. Kaspi, Michael Kramer, Maura A. McLaughlin, Maxim Lyutikov, Scott M. Ransom, Ingrid H. Stairs, Robert D. Ferdman, Fernando Camilo, Andrea Possenti. 2008-07-16. Relativistic Spin Precession in the Double Pulsar. https://doi.org/10.1126/scien%3D

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