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Abstract
A generalized analysis of the local entropy production of a simple fluid is used to show that, if intrinsic angular momentum is taken into account, rotational viscosity must arise in the linear non-equilibrium regime. As a consequence, the stress tensor of dense rotating matter, such as the one present in neutron stars, posseses a significant non-vanishing antisymmetrical part. A simple argument suggests that, due to the extreme magnetic fields present in neutron stars, the relaxation time associated to rotational viscosity is large (∼1021). The formalism leads to generalized Navier-Stokes equations useful in neutron star physics which involve vorticity in the linear regime.
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Published Online: 2005-06-01
Published in Print: 2001-09-11
Copyright © 2001 by Walter de Gruyter GmbH & Co. KG
