Relativistic spin precession in the double pulsar.
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 .65)(+0 degrees .66) per year (68% confidence level) is consistent with that predicted by general relativity within an uncertainty of 13%.
Breton
Rene P
RP
Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada. bretonr@physics.mcgill.ca
Kaspi
Victoria M
VM
Kramer
Michael
M
McLaughlin
Maura A
MA
Lyutikov
Maxim
M
Ransom
Scott M
SM
Stairs
Ingrid H
IH
Ferdman
Robert D
RD
Camilo
Fernando
F
Possenti
Andrea
A