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Alfredo Sandoval-Villalbazo, Ana Laura García-Perciante, L. S. García Colín

Rotational Viscosity in Linear Irreversible Thermodynamics and its Application to Neutron Stars

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.

Journal of Non-Equilibrium Thermodynamics, Walter de Gruyter

Print ISSN: 0340-0204
Volume: 26, 09/2001
Pages: 269 - 277

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