Fast fossil rotation of neutron star cores

Understand

It is argued that the superfluid core of a neutron star super-rotates relative to the crust, because stratification prevents the core from responding to the electromagnetic braking torque, until the relevant dissipative (viscous or Eddington-Sweet) time-scale, which can exceed ~ 10^3 yr and is much longer than the Ekman timescale, has elapsed.

• Hence, in some young pulsars, the rotation of the core today is a fossil record of its rotation at birth, provided that magnetic crust-core coupling is inhibited, e.g.
• by buoyancy, field-line topology, or the presence of uncondensed neutral components in the superfluid.
• Persistent core super-rotation alters our picture of neutron stars in several ways, allowing for magnetic field generation by ongoing dynamo action and enhanced gravitational wave emission from hydrodynamic instabilities.