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

Alfredo Sandoval-Villalbazo·Ana Garcia-Perciante·LS Garcia-Colin
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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-vansishing 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 (approx 10^{21} s). The formalism leads to generalized Navier-Stokes equations useful in neutron star physics which involve vorticity in the linear regime.

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Alfredo Sandoval-Villalbazo, Ana Garcia-Perciante, LS Garcia-Colin. 2001-02-27. Rotational Viscosity in Linear Irreversible Thermodynamics and its Application to Neutron Stars. https://doi.org/10.1515/jnetdy.2001.019

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