  We describe the morphological and fluctuation properties of the pulsars in
the double neutron star system, PSR J0737--3039. Pulsar B is seen in almost all
orbital phases, except in the range of $\sim 6\deg$ to $65\deg$. This may be
interpreted as an {\it eclipse} of pulsar B's signal by its own magnetopause
region produced by interaction with pulsar A's relativistic wind. No modulation
of the emission of pulsar B is found at the period of pulsar A. This places a
constraint on the models that propose that pulsar A's beamed radiation is
directly responsible for pulsar B's emission. Modulation index values indicate
that the pulse to pulse variations in the two objects are mostly intrinsic.
Pulsar A shows significant differential modulation index within its pulse
profile.
