Volume 438, Number 2, August I 2005
|Page(s)||643 - 651|
|Section||Stellar structure and evolution|
|Published online||08 July 2005|
Instabilities, turbulence, and mixing in the ocean of accreting neutron stars
Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain A.F.Ioffe Institute for Physics and Technology and Isaak Newton Institute of Chili, Branch in St. Petersburg, 194021 St. Petersburg, Russia e-mail: email@example.com
Accepted: 17 March 2005
We consider the stability properties of the ocean of accreting magnetic neutron stars. It turns out that the ocean is always unstable due to the combined influence of the temperature and chemical composition gradients along the surface and of the Hall effect. Both the oscillatory and non-oscillatory modes can be unstable in accreting stars. The oscillatory instability grows on a short timescale ~ s depending on the lengthscale of a surface inhomogeneity and the wavelength of perturbations. The instability of non-oscillatory modes is typically much slower and can develop on a timescale of hours or days. Instability generates a weak turbulence that can be responsible for mixing between the surface and deep ocean layers and for spreading the accreted material over the stellar surface. Spectral features of heavy elements can be detected in the atmospheres of accreting stars due to mixing, and these features should be different in neutron stars with both stable and unstable burning. Motions caused by instability can also be the reason for slow variations in the luminosity.
Key words: magnetohydrodynamics (MHD) / convection / stars: neutron / stars: magnetic fields
© ESO, 2005
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