On the Peculiar Rotational Evolution of PSR B0950+08

TL;DR

This paper proposes a model explaining the sinusoidal-like oscillations in the spin-down rate of pulsar PSR B0950+08 through vortex line dynamics and internal temperature effects, linking internal superfluid behavior to observable rotational variations.

Contribution

It introduces a novel model connecting vortex line oscillations and internal temperature to the pulsar's rotational evolution, providing insights into neutron star interior properties.

Findings

The model reproduces observed spin-down oscillations in PSR B0950+08.

Internal temperature influences vortex pinning and creep behavior.

Oscillation periods can constrain the magnetic field structure in neutron star cores.

Abstract

The long-term rotational evolution of the old, isolated pulsar, PSR B0950+08 is intriguing in that its spin-down rate displays sinusoidal-like oscillations due to alternating variations, both in magnitude and sign, of the second time derivative of the pulse frequency. We show that the large internal temperature to pinning energy ratio towards the base of the crust implied by the recent high surface temperature measurement of PSR B0950+08 leads to linear creep interaction between vortex lines and pinning sites to operate in this pulsar. Vortex lines assume a parabolic shape due to pinning to nuclear clusters and finite tension of vortices acts as a restoring force that tends to bring a vortex back to its straight shape. The resulting low frequency oscillations of vortex lines combined with the time variable coupling between the internal superfluid components and the external pulsar braking torque give rise to an oscillatory spin-down rate. We apply this model to PSR B0950+08 observations for several external torque models. Our model has potential to constrain the radial extension of the closed magnetic field region in the outer core of neutron stars from the oscillation period of the spin-down rate.