  We report timing results for PSR J2234+0611, a 3.6-ms pulsar in a 32-day,
eccentric (e = 0.13) orbit with a helium white dwarf companion discovered as
part of the Arecibo Observatory 327 MHz drift scan survey. The precise timing
and the eccentric nature of the orbit allow precise measurements of an unusual
number of parameters: a) a precise proper motion of 27.10(3) mas/yr and a
parallax of 1.05(4) mas resulting in a pulsar distance of 0.95(4) kpc; this
allows a precise estimate of the transverse velocity, 123(5) km/s. Together
with previously published spectroscopic measurements of the systemic radial
velocity, this allows a full 3-D determination of the system's velocity; b)
precise measurements of the rate of advance of periastron, which after
subtraction of the contribution of the proper motion yields a total system mass
of $1.6518^{+0.0033}_{-0.0035}$ solar masses; c) a Shapiro delay measurement,
h_3 = $82 \pm 14$ ns despite the orbital inclination not being near 90 deg;
combined with the measurement of the total mass, this yields a pulsar mass of
$1.353^{+0.014}_{-0.017}$ solar masses and a companion mass of
$0.298^{+0.015}_{-0.012}$ solar masses; d) we measure precisely the secular
variation of the projected semi-major axis and detect significant annual
orbital parallax; together these allow a determination of the full 3-D orbital
geometry, including an unambiguous orbital inclination (i =
$138.7^{+2.5}_{-2.2}$ deg) and a position angle for the line of nodes (Omega =
$44^{+5}_{-4}$ deg). We discuss the component masses to investigate hypotheses
previously advanced to explain the origin of eccentric MSPs. The unprecedented
determination of the full 3-D position, motion and orbital orientation of the
system, plus the precisely measured pulsar and WD mass and the latter's optical
detection make this system an unique test of our understanding of white dwarfs
and their atmospheres.
