Shear Viscosity of the outer crust of Neutron stars: Ion Contribution

Simple item page
dc.creatorCaballero, O. L.
dc.creatorPostnikov, S.
dc.creatorHorowitz, C. J.
dc.creatorPrakash, M.
dc.date2008-07-28
dc.date2008-10-30
dc.date.accessioned2026-07-07T11:45:07Z
dc.date.available2026-07-07T11:45:07Z
dc.descriptionThe shear viscosity of the crust might have a damping effect on the amplitude of r-modes of rotating neutron stars. This damping has implications for the emission of gravitational waves. We calculate the contribution to the shear viscosity coming from the ions using both semi-analytical methods, that consider binary collisions, and Molecular Dynamics simulations. We compare these results with the contribution coming from electrons. We study how the shear viscosity depends on density for conditions of interest in neutron star envelopes and outer crusts. In the low density limit, we find good agreement between results of our molecular dynamics simulations and classical semi-analytic calculations.
dc.description13 pages, 14 figures, Subsection added
dc.identifierhttps://arxiv.org/abs/0807.4353
dc.identifierhttp://arxiv.org/abs/0807.4353
dc.identifierPhys.Rev.C78:045805,2008
dc.identifierdoi:10.1103/PhysRevC.78.045805
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/201779
dc.subjectAstrophysics
dc.subjectNuclear Theory
dc.titleShear Viscosity of the outer crust of Neutron stars: Ion Contribution
dc.typetext

Files

Collections

arXiv