A Non-Radial Oscillation Model for Pulsar State Switching

TL;DR

This paper proposes a non-radial oscillation model to explain quasi-periodic timing noise in pulsars, linking pulsar interior dynamics to observed spin-down fluctuations and pulse profile changes, potentially enhancing pulsar timing accuracy.

Contribution

It introduces a novel asteroseismology-based model for pulsar timing noise, connecting internal oscillations to observable timing and profile variations.

Findings

The model explains quasi-periodic fluctuations in pulsar spin-down rates.

Application of the model can improve pulsar timing precision.

Provides insights into neutron star interiors through oscillation analysis.

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.