Arrival-time analysis for a pulsar in a binary system

A method is described for analyzing the arrival times of pulses from the binary pulsar PSR 1913+16, in terms of the orbital elements and their possible secular variations. Estimates are given for the times necessary to measure such secular changes and to detect various relativistic effects. If measurements errors approx.1 ms are the dominant source of error and approx.1000 independent observations are made per year, then approx.5 years of observations are necessary for a dynamical determination of the component masses accurate to 10 percent and approx.15 years for the possible detection of gravitational radiation. Other sources of error are briefly discussed. (AIP)