Shear modulus of neutron star crust

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Shear modulus of neutron star crust

The shear modulus of solid neutron star crust is calculated by the thermodynamic perturbation theory, taking into account ion motion. At a given density, the crust is modelled as a bodycentred cubic Coulomb crystal of fully ionized atomic nuclei of one type with a uniform charge-compensating electron background. Classic and quantum regimes of ion motion are considered. The calculations in the c...

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Shear Viscosity and Oscillations of Neutron Star Crust

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 ∼10 g/cm to 10–10 g/cm we consider the matter composed of widely abundant astrophysical elements, fromH to Fe. For higher densities, 10–10 g/cm, we employ the ground-state nuclear comp...

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Durability of Neutron Star Crust

How long do neutron star mountains last? The durability of elastically deformed crust is important for neutron star physics including pulsar glitches, emission of gravitational waves from static mountains, and flares from star quakes. The durability is defined by the strength properties of the Yukawa crystals of ions, which make up the crust. In this paper we extend our previous results [Mon. N...

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Coulomb crystals in neutron star crust

It is well known that neutron star crust in a wide range of mass densities and temperatures is in a crystal state. At a given density, the crystal is made of fully ionized atomic nuclei of a single species immersed in a nearly incompressible (i.e., constant and uniform) charge compensating background of electrons. This model is known as the Coulomb crystal model. In this talk we analyze thermod...

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ژورنال

عنوان ژورنال: Monthly Notices of the Royal Astronomical Society

سال: 2011

ISSN: 0035-8711

DOI: 10.1111/j.1365-2966.2011.18819.x