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We present radio pulsar emission beam analyses and models with the primaryintent of examining pulsar beam geometry and physics over the broadest band ofradio frequencies reasonably obtainable. We consider a set of well-studiedpulsars that lie within the Arecibo sky. These pulsars stand out for the broadfrequency range over which emission is detectable, and have been extensivelyobserved at frequencies up to 4.5 GHz and down to below 100 MHz. We utilizepublished profiles to quantify a more complete picture of the frequencyevolution of these pulsars using the core/double-cone emission beam model asour classification framework. For the low-frequency observations, we take intoaccount measured scattering time-scales to infer intrinsic vs scatterbroadening of the pulse profile. Lastly, we discuss the populational trends ofthe core/conal class profiles with respect to intrinsic parameters. Wedemonstrate that for this sub-population of pulsars, core and conal dominatedprofiles cluster together into two roughly segregated $P$-$\dot{P}$populations, lending credence to the proposal that an evolution in thepair-formation geometries is responsible for core/conal emission and otheremission effects such as nulling and mode-changing.

Pulsar Emission Beam Geometry of Radio Broadband Arecibo Sources