G. J. Qiao

Pulsar rotation measures and the magnetic structure of our Galaxy

We have obtained 63 rotation measures (RMs) from polarization observations of southern pulsars, of which 54 are new measurements and three are varied from previous values. The new pulsar RM data at high Galactic latitudes are mostly consistent with the antisymmetric RM distribution found previously. For the Galactic disc, evidence for a field reversal near the Perseus arm, and possibly another beyond it, is presented. Inside the Solar Circle, in addition to the two known field reversals in or near the Carina–Sagittarius arm and the Crux–Scutum arm, a further reversal in the Norma arm is tentatively identified. These reversals, together with the pitch angle derived from pulsar RM and stellar polarization distributions, are consistent with bisymmetric spiral models for the large-scale magnetic field structure in the disc of our Galaxy. However, discrimination between models is complicated by the presence of smaller scale irregularities in the magnetic field, as well as uncertainties in the theoretical modelling.

Detection of 107 glitches in 36 southern pulsars

Timing observations from the Parkes 64-m radio telescope for 165 pulsarsbetween 1990 and 2011 have been searched for period glitches. Data spansfor each pulsar ranged between 5.3 and 20.8 yr. From the total of 1911yr of pulsar rotational history, 107 glitches were identified in 36pulsars. Out of these glitches, 61 have previously been reported whereas46 are new discoveries. Glitch parameters, both for the previously knownand the new glitch detections, were measured by fitting the timingresidual data. Observed relative glitch sizes{

Circular polarization in pulsar integrated profiles

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WIND BRAKING OF MAGNETARS

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Pulsar Braking Index: A Test of Emission Models?

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The inner annular gap for pulsar radiation: gamma-ray and radio emission

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Counterclockwise Magnetic Fields in the Norma Spiral Arm

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What if pulsars are born as strange stars

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The annular gap model for γ‐ray emission from young and millisecond pulsars

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The formation of submillisecond pulsars and the possibility of detection

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