EDP Sciences
Free access
Volume 421, Number 1, July I 2004
Page(s) L5 - L8
Section Letters
DOI http://dx.doi.org/10.1051/0004-6361:20040165

A&A 421, L5-L8 (2004)
DOI: 10.1051/0004-6361:20040165


Neutron star oceans: Instability, mixing, and heat transport

V. Urpin

Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain A.F.Ioffe Institute of Physics and Technology and Isaak Newton Institute of Chili, Branch in St. Petersburg, 194021 St. Petersburg, Russia

(Received 8 March 2004 / Accepted 10 May 2004)

Stability of the ocean of magnetic neutron stars is considered. We argued that the ocean is unstable if the temperature varies along the surface. The instability grows on a time scale ~ 0.1-100 s depending on the lengthscale of perturbations and generates a weak turbulence. Turbulence can be responsible for mixing between the surface and deep ocean layers and can enhance heat transport in the surface region.

Key words: MHD -- convection -- stars: neutron -- instabilities

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