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Shear viscosity and oscillations of neutron star crust

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Abstract

We calculate the electron shear viscosity of dense matter (determined by Coulomb electron collisions) in a wide range of parameters typical for white dwarf cores and neutron star crusts. In the density range from ∼103 g/cm3 to 107–1010 g/cm3 we consider the matter composed of widely abundant astrophysical elements, from H to Fe. For higher densities, 1010–1014 g/cm3, we employ the ground-state nuclear composition, taking into account finite sizes of atomic nuclei and the distribution of proton charge over the nucleus. Numerical values of the viscosity are approximated by an analytic expression convenient for applications. Using the approximation of plane-parallel layer, we study frequencies, eigenmodes, and viscous damping times of oscillations of high multipolarity, l ∼ 500–1000, localized in the outer crust of a neutron star. For instance, at l ∼ 500 oscillations have frequencies f ≳ 40 kHz and are localized not deeper than about 300 m from the surface. When the crust temperature decreases from 109 K to 107 K, the dissipation time of these oscillations (with a few radial nodes) decreases from ∼1 year to 10–15 days.

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Authors and Affiliations

  1. Ioffe Physicotechnical Institute, St. Petersburg, Russia

    A. I. Chugunov & D. G. Yakovlev

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  1. A. I. Chugunov
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  2. D. G. Yakovlev
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__________

Translated from Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l}\) Zhurnal, Vol. 82, No. 9, 2005, pp. 814–829.

Original Russian Text Copyright © 2005 by Chugunov, Yakovlev.

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Chugunov, A.I., Yakovlev, D.G. Shear viscosity and oscillations of neutron star crust. Astron. Rep. 49, 724–738 (2005). https://doi.org/10.1134/1.2045323

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