Abstract:
General relativistic effects due to spacetime curvature and rotation on the arrival times of pulsar signals are investigated using a rotationally perturbed spherical metric. It is found that for the millisecond pulsar PSR 1937+214, the advancement in arrival time (assuming the usual polar cap model for emission mechanism and a radius-to-frequency mapping) due to these effects is nontrivial. The results are compared with recent multifrequency timing measurements on PSR 1937+214, and the implications regarding emission region thickness and emission mechanism for fast pulsars are pointed out.
