On the pulsar spin frequency derivatives and the glitch activity

TL;DR

This paper investigates how pulsar spin frequency derivatives relate to glitch activity, proposing a new method to quantify glitch activity using these derivatives and providing insights into neutron star interior dynamics.

Contribution

It introduces a novel approach to estimate pulsar glitch activity from spin frequency derivatives, linking glitch behavior to neutron star crust superfluid properties.

Findings

The ratio | u|/ u^2 constrains glitch activity.

Lower values of the ratio correlate with more glitches.

The inner-crust superfluid's moment of inertia is at most 10% of the star's total.

Abstract

The number of sudden spin-ups in radio pulsars known as pulsar glitches has increased over the years. Though a consensus has not been reached with regards to the actual cause of the phenomenon, the electromagnetic braking torque on the crust quantified via the magnitude of pulsar spin frequency first derivative, $ \dot{\nu} $ is a key factor in mechanisms put across toward the understanding of the underlying principles involved. The glitch size has been used to establish a quantity used to constrain the mean possible change in pulsar spin frequency $ (\nu) $ per year due to a glitch known as the `glitch activity'. Traditionally, the glitch activity parameter $ A_{g} $ is calculated from the cumulative glitch sizes in a pulsar at a certain observational time span. In this analysis, we test the possibility of of quantifying the $ A_{g} $ with the pulsars main spin frequency derivatives (i.e. $ \dot{\nu} $ and $\ddot{\nu} $). In this approach, the ratio of the frequency derivatives, i.e. $ |\ddot{\nu}|/\dot{\nu}^{2} $ is seen to constrains the glitch activity in radio pulsars. The glitch size is found to be independent of the magnitude of the ratio, however, based on the recorded glitch events, the lower end of $ |\ddot{\nu}|/\dot{\nu}^{2} $ distribution appear to have more glitches. The minimum inter-glitch time interval in the ensemble of pulsars scale with the ratio as $t_{g} \sim 3.35(|\ddot{\nu}|/\dot{\nu}^{2})^{0.23} $. The $ A_{g} $ quantified in this analysis supports the idea of neutron star inner-crust superfluid being the reservoir of momentum transferred during glitches. It suggests that the moment of inertia of the inner-crust to be at most 10 % of the entire neutron star moment of inertia.