  Radio pulsar B1933+16 is brightest core-radiation dominated pulsar in the
Arecibo sky, and here we carry out a comprehensive high resolution polarimetric
study of its radiation at both 1.5 and 4.6 GHz. At 1.5 GHz, the polarization is
largely compatible with a rotating-vector model with $\alpha$ and $\beta$
values of 125 and --1.2$^{\circ}$, such that the core and conal regions can be
identified with the primary and secondary polarization modes and plausibly with
the extraordinary and ordinary propagation modes. Polarization modal
segregation of profiles shows that the core is comprised of two parts which we
associate with later X-mode and earlier O-mode emission. Analysis of the broad
microstructures under the core shows that they have similar timescales to those
of the largely conal radiation of other pulsars studied earlier.
Aberration/retardation analysis was here possible for both the conal and core
radiation and showed average physical emission heights of about 200 km for
each. Comparison with other core-cone pulsars suggests that the core and conal
emission arises from similar heights. Assuming the inner vacuum gap model, we
note that at these emission altitudes the frequency of the observed radiation
$\nu_{obs}$ is less than the plasma frequency $\nu_p$. We then conclude that
the radio emission properties are consistent with the theory of coherent
curvature radiation by charged solitons where the condition $\nu_{obs} <
\nu_{p}$ is satisfied. However, the differences that exist between core and
conal emission in their geometric locations within a pulse, polarization and
modulation properties are yet to be understood.
