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We study the bi-drifting pulsar B1839-04, where the observed subpulse driftdirection in the two leading pulse components is opposite from that in the twotrailing components. Such diametrically opposed apparent motions challenge ourunderstanding of an underlying structure. We find that for the geometry spannedby the observer and the pulsar magnetic and rotation axes, the observedbi-drifting in B1839-04 can be reproduced assuming a non-dipolar configurationof the surface magnetic field. Acceptable solutions are found to either haverelatively weak $(\sim 10^{12} \,{\rm G})$ or strong $(\sim 10^{14} \,{\rm G})$surface magnetic fields. Our single pulse modeling shows that a global electricpotential variation at the polar cap that leads to a solid-body-like rotationof spark forming regions is favorable in reproducing the observed driftcharacteristics. This variation of the potential additionally ensures that thevariability is identical in all pulse components resulting in the observedphase locking of subpulses. Thorough and more general studies of pulsargeometry show that a low ratio of impact factor to opening angle $(\beta /\rho)$ increases the likelihood of bi-drifting to be observed. We thus concludethat bi-drifting is visible when our line of sight crosses close to themagnetic pole.

Single pulse modeling and the bi-drifting subpulses of radio pulsar B1839-04