Superfluid neutron star turbulence
Superfluid neutron star turbulence
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 polarized 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 polarized turbulent system.
hydrodynamics, turbulence, stars: neutron
747-756
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Sidery, Trevor
eadf965c-ecfe-40af-94f5-19e88d301b02
Comer, Greg L
e78ae434-e576-4b39-93cd-679b6f30432d
October 2007
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Sidery, Trevor
eadf965c-ecfe-40af-94f5-19e88d301b02
Comer, Greg L
e78ae434-e576-4b39-93cd-679b6f30432d
Andersson, Nils, Sidery, Trevor and Comer, Greg L
(2007)
Superfluid neutron star turbulence.
Monthly Notices of the Royal Astronomical Society, 381 (2), .
(doi:10.1111/j.1365-2966.2007.12251.x).
Abstract
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 polarized 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 polarized turbulent system.
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Published date: October 2007
Keywords:
hydrodynamics, turbulence, stars: neutron
Identifiers
Local EPrints ID: 54971
URI: http://eprints.soton.ac.uk/id/eprint/54971
ISSN: 1365-2966
PURE UUID: 970c9f2e-3fe4-4b87-bcad-91d0e8a82e0c
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Date deposited: 28 Jul 2008
Last modified: 16 Mar 2024 03:02
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Author:
Trevor Sidery
Author:
Greg L Comer
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