A Non-Radial Oscillation Model for Pulsar State Switching

Abstract

Pulsars are unique astrophysical laboratories because of their clock-like timing precision, providing new ways to test general relativity and detect gravitational waves. One impediment to high-precision pulsar timing experiments is timing noise. Recently Lyne et al. (2010) showed that the timing noise in a number of pulsars is due to quasi-periodic fluctuations in the pulsars' spin-down rates and that some of the pulsars have associated changes in pulse profile shapes. Here we show that a non-radial oscillation model based on asteroseismological theory can explain these quasi-periodic fluctuations. Application of this model to neutron stars will increase our knowledge of neutron star emission and neutron star interiors and may improve pulsar timing precision.

13 pages, 2 figures, 1 tables, Accepted for publication in ApJ Letters

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• Long-term Radio Observations of the Intermittent Pulsar B1931+24
• On the Pulse Intensity Modulation of PSR B0823+26
• Pulsar wind model for the spin-down behavior of intermittent pulsars
• Evidence for chaotic behaviour in pulsar spin-down rates
• Radio Properties of Rotating Radio Transients I: searches for periodicities and randomness in pulse arrival times
• Particle acceleration in the polar cap region of an oscillating neutron star
• Individual pulse emission from the diffuse drifter PSR J1401$-$6357 using the ultrawideband receiver on the Parkes radio telescope