Investigations of the emission geometry of the four-component radio pulsar J0631+1036

Radio pulsar J0631+1036 presents a remarkably clear example of a rare fourcomponent profile, and with apparently large aberration/retardation indicated by its linear polarization-angle traverse, but on closer study its profiles are difficult to understand and interpret. Given the broad success of the core/double-cone geometric model in describing the profiles of slower pulsars, we assess whether it could be appropriate for J0631+1036. The emission geometry resulting from application of this model is not implausible; however, it is difficult to reconcile it with the well resolved forms of the inner component pair. Overall, we are forced to conclude that this pulsar emits somewhat differently than its closest peers, perhaps because it is located within a dense star-forming region. Both a bi-directional emission model and a “wedge” model are discussed as alternatives.