  We report on 12 years of observations of PSR J1713+0747, a pulsar in a 68-day
orbit with a white dwarf. Pulse times of arrival were measured with
uncertainties as small as 200 ns. The timing data yielded measurements of the
relativistic Shapiro delay, perturbations of pulsar orbital elements due to
secular and annual motion of the Earth, and the pulsar's parallax, as well as
pulse spin-down, astrometric, and Keplerian measurements. The observations
constrain the masses of the pulsar and secondary star to be m1=1.3+-0.2 solar
masses and m2=0.28+-0.03 solar masses, respectively (68% confidence). Combining
the theoretical orbital period-core mass relation with the observational
constraints yields a somewhat higher pulsar mass, m1=1.53-0.06+0.08 solar
masses. The parallax is 0.89+-0.08 mas, corresponding to a distance of 1.1+-0.1
kpc; the precision of the parallax measurement is limited by uncertainties in
the electron content of the solar wind. The transverse velocity is unusually
small, 33+-3 km/s. We find significant timing noise on time scales of several
years, but no more than expected by extrapolating timing noise statistics from
the slow pulsar population. With the orientation of the binary orbit fully
measured, we are able to improve on previous tests of equivalence principle
violations.

Astrophysics