On the peculiar rotational evolution of PSR B0950+08

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.

Automated summary

The long-term rotational evolution of the old, isolated pulsar, PSR B0950+08, displays sinusoidal-like oscillations in its spin-down rate due to alternating variations in the second time derivative of the pulse frequency. This can be explained by the linear creep interaction between vortex lines and pinning sites in the pulsar, which is influenced by the large internal temperature to pinning energy ratio. The oscillatory spin-down rate can help constrain the radial extension of the closed magnetic field region in the outer core of neutron stars.