  Our recent studies of pulsar population statistics suggest that improvements
of radio and gamma-ray beam geometry and luminosity models require further
refinement. The goal of this project is to constrain the viewing geometry for
some radio pulsars, especially three-peaked pulse profiles, in order to limit
the uncertainty of the magnetic inclination and impact angles. We perform fits
of the pulse profile and position angle sweep of radio pulsars for the
available frequencies. We assume a single core and conal beams described by
Gaussians. We incorporate three different size cones with frequency dependence
from the work of Mitra & Deshpande (1999). We obtain separate spectral indices
for the core and cone beams and explore the trends of the ratio of core to cone
peak fluxes. This ratio is observed to have some dependence with period.
However, we cannot establish the suggested functional form of this ratio as
indicated by the work of Arzoumanian, Chernoff & Cordes (2002).
