The large-scale magnetic field of our Galaxy can be probed in three dimensions using Faraday rotation of pulsar signals. We report on the determination of 223 rotation measures from polarization observations of relatively distant southern pulsars made using the Parkes radio telescope. Combined with previously published observations these data give clear evidence for large-scale counterclockwise fields (viewed from the north Galactic pole) in the spiral arms interior to the Sun and weaker evidence for a counterclockwise field in the Perseus arm. However, in interarm regions, including the Solar neighbourhood, we present evidence that suggests that large-scale fields are clockwise. We propose that the large-scale Galactic magnetic field has a bisymmetric structure with reversals on the boundaries of the spiral arms. Streaming motions associated with spiral density waves can directly generate such a structure from an initial inwardly directed radial field. Large-scale fields increase toward the Galactic Center, with a mean value of about 2~$\mu$G in the Solar neighbourhood and 4~$\mu$G at a Galactocentric radius of 3 kpc.
A new single pulse behaviour has been identified in two pulsars, B0919+06 and B1859+07. Normally both starts emit bright subpulses in a region near the trailing edge of heir profile. However, occasionally these stars exhibit "events" wherein the emission longitude gradually decreases by about their profile width, remains in this position for typically tens of pulses and then gradually returns over a few pulses to the usual longitude. The effect bears some resemblance to a profile "mode change", but here the effect is gradual and episodic. When the separated profiles of the normal and "event" emission, they reveal a broad and complex profile structure in each pulsar - but one which can probably be understood correctly in terms of a single conical beam. Possibly the effect entails an extreme example of "absorption"-induced profile asymmetry, as suspected in other pulsars. Alternatively, shifting sources of illumination within the pulsar beam may be responsible.
Neutron stars are discussed as laboratories of physics of strong gravitational fields. The mass of a neutron star is split into matter energy and gravitational field energy contributions. The energy of the gravitational field of neutron stars is calculated with three different approaches which give the same result. It is found that up to one half of the gravitational mass of maximum mass neutron stars is comprised by the gravitational field energy. Results are shown for a number of realistic equations of state of neutron star matter.