Topology and Polarisation of Subbeams Associated With Pulsar 0943+10's ``Drifting''-Subpulse Emission: I. Analysis of Arecibo 430- and 111-MHz Observations

The drifting'' subpulses exhibited by some radio pulsars have fascinated both observers and theorists for 30 years, and have been widely regarded as one of the most critical and potentially insightful aspects of their emission. Here, we report on detailed studies of pulsar B0943+10, whose nearly coherent sequences of drifting’’ subpulses have permitted us to identify their origin as a system of subbeams that appear to circulate around the star’s magnetic axis. We introduce several new techniques of analysis, and we find that both the primary and secondary features in the star’s fluctuation spectra are aliases of their actual values. We have also developed a method of tracing the underlying pattern responsible for the observed sequences, using a cartographic'' transform and its inverse, permitting us to study the characteristics of the polar-cap emission map’’ and to confirm that such a map'' in turn represents the observed sequence. We apply these techniques to the study of three different Arecibo observations. The B’‘-mode sequences are consistent in revealing that the emission pattern consists of 20 subbeams, which rotate around the magnetic axis in about 37 periods or 41 seconds. Even in the Q'' mode sequence, we find evidence of a compatible circulation time. The similarity of the subbeam patterns at different radio frequencies strongly suggests that the radiation is produced within a set of columns, which extend from close to the stellar surface up though the emission region and reflect some manner of a seeding’'phenomenon at their base. The subbeam emission is then tied neither to the stellar surface nor to the field.