  General relativity predicts that the spin axes of the pulsars in the
double-pulsar system (PSR J0737-3039A/B) will precess rapidly, in general
leading to a change in the observed pulse profiles. We have observed this
system over a one-year interval using the Parkes 64-m radio telescope at three
frequencies: 680, 1390 and 3030 MHz. These data, combined with the short survey
observation made two years earlier, show no evidence for significant changes in
the pulse profile of PSR J0737-3039A, the 22-ms pulsar. The limit on variations
of the profile 10% width is about 0.5 deg per year. These results imply an
angle delta between the pulsar spin axis and the orbit normal of <~ 60 deg,
consistent with recent evolutionary studies of the system. Although a wide
range of system parameters remain consistent with the data, the model proposed
by Jenet & Ransom (2004) can be ruled out. A non-zero ellipticity for the
radiation beam gives slightly but not significantly improved fits to the data,
so that a circular beam describes the data equally well within the
uncertainties.
