Superfluid neutron star turbulence

Details Superfluid neutron star turbulence Superfluid neutron star turbulence

2007-03-12

arxiv.org/abs/astro-ph/0703257v1

Astronomy and Astrophysics

Astrophysics

15 pages, 2 figures

Scientific paper

10.1111/j.1365-2966.2007.12251.x

We analyse the implications of superfluid turbulence for neutron star physics. We begin by extending our previous results for the mutual friction force for a straight vortex array to account for the self-induced flow which arises when the vortices are curved. We then discuss Vinen's phenomenological model for isotropic turbulence, and derive the associated (Gorter-Mellink) form for the mutual friction. We compare this derivation to a more recent analysis of Schwarz, which sheds light on various involved issues. Having discussed isotropic turbulence, we argue that this case is unlikely to be relevant for neutron stars. Instead we expect a rotating neutron star to exhibit polarised turbulence, where relative flow drives the turbulence and rotation counteracts it. Based on recent results for superfluid Helium, we construct a phenomenological model that should have the key features of such a polarised turbulent system.

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