  The sizes of pulsar radio pulses in the plane of the sky are determined. This
is important not only in relation to the possibility of directly resolving the
radio pulses spatially, but also for verifying and placing constraints on
existing theories of the radio emission. The shape of the pulse radio image and
its variation as a function of the pulse phase for the extraordinary (X) and
ordinary (O) modes are determined for the simple case of a dipolar magnetic
field. Images are obtained for pulsars with various angles between their
magnetic and rotational axes, and also for various model parameters, such as
the height of the emission, the size of the emission region as a function of
the height, and the Lorentz factor of the secondary plasma. It is shown that
the size of the resulting image is appreciably smaller at the center of the
pulse than at its edges.
