  We present radio pulsar emission beam analyses and models with the primary
intent of examining pulsar beam geometry and physics over the broadest band of
radio frequencies reasonably obtainable. We consider a set of well-studied
pulsars that lie within the Arecibo sky. These pulsars stand out for the broad
frequency range over which emission is detectable, and have been extensively
observed at frequencies up to 4.5 GHz and down to below 100 MHz. We utilize
published profiles to quantify a more complete picture of the frequency
evolution of these pulsars using the core/double-cone emission beam model as
our classification framework. For the low-frequency observations, we take into
account measured scattering time-scales to infer intrinsic vs scatter
broadening of the pulse profile. Lastly, we discuss the populational trends of
the core/conal class profiles with respect to intrinsic parameters. We
demonstrate that for this sub-population of pulsars, core and conal dominated
profiles cluster together into two roughly segregated $P$-$\dot{P}$
populations, lending credence to the proposal that an evolution in the
pair-formation geometries is responsible for core/conal emission and other
emission effects such as nulling and mode-changing.
