The traditional, geometrical rotating vector model (RVM) has proved particularly poor at capturing the polarization sweeps of the young energetic and millisecond pulsars detected by \textit{Fermi}. We augment this model by including finite altitude effects using a swept back vacuum dipole geometry. By further including the effects of orthogonal mode jumps, multiple emission altitudes, open zone growth via y-point lowering, and interstellar scattering, we show that a wide range of departures from RVM can be modeled well while retaining a geometrical picture. We illustrate these effects by fitting six \textit{Fermi}-detected pulsars (J0023+0923, J1024−0719, J1744−1134, J1057−5226, J1420−6048, and J2124−3358) and we describe how such modeling can improve our understanding of their emission geometry.
@article{arxiv.1408.3682,
title = {Tackling Radio Polarization of Energetic Pulsars},
author = {H. A. Craig},
journal= {arXiv preprint arXiv:1408.3682},
year = {2015}
}