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Description
Radio emission from pulsars is commonly modelled as a core and cone beam, since this decomposition reasonably reproduces the single, double, and multiple-component pulse profiles observed across the pulsar population, unlike a simple single-beam model. This structure is usually modelled within a vacuum dipole magnetic field. However, this is inconsistent with the more modern force-free magnetosphere, where plasma-filled conditions alter the global magnetic field structure and the geometry of the open field line region, changing the size and location of the core and cone components. In this work, we implement the core and cone beam geometry assuming a force-free magnetosphere. We perform a study to simulate radio light curves and constrain the core and cone beam widths and their relative luminosity, along with the magnetic inclination angle and observer angle for a sample of young pulsars. The goal is to test whether the core and cone geometry reproduces observed pulse shapes and to eventually incorporate it in dual-band light curve fits that also include gamma-ray light curves. We will lastly use these light curve fits to uncover trends across a population of bright, radio-loud Fermi LAT $\gamma$-ray pulsars.