Instability of Superfluid Flow in the Neutron Star Core

Details Instability of Superfluid Flow in the Neutron Star Core Instability of Superfluid Flow in the Neutron Star Core

2011-11-03

arxiv.org/abs/1111.0696v3

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

12 pages. Final journal version

Scientific paper

Pinning of superfluid vortices to magnetic flux tubes in the outer core of a neutron star supports a velocity difference of $\sim 10^5$ \cms\ between the neutron superfluid and the proton-electron fluid as the star spins down. Under the Magnus force that arises on the vortex array, vortices undergo {\em vortex creep} through thermal activation or quantum tunneling. We examine the hydrodynamic stability of this situation. Vortex creep introduces two low-frequency modes, one of which is unstable above a critical wavenumber for any non-zero flow velocity of the neutron superfluid with respect to the charged fluid. For typical pinning parameters of the outer core, the superfluid flow is unstable over wavelengths $\lambda\lap 10$ m and over timescales of $\sim (\lambda/{1 m})^{1/2}$ yr down to $\sim 1$ d. The vortex lattice could degenerate into a tangle, and the superfluid flow would become turbulent. We suggest that superfluid turbulence could be responsible for the red timing noise seen in many neutron stars, and find a predicted spectrum that is generally consistent with observations.

Affiliated with

Also associated with

No associations

Rating

Instability of Superfluid Flow in the Neutron Star Core does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Instability of Superfluid Flow in the Neutron Star Core, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Instability of Superfluid Flow in the Neutron Star Core will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-700645