Abstract
The aim of the present paper will be to derive the fundamental equations for rotation about the centre of gravity of a celestial body, consisting of material of arbitrary viscosity, in an external field.
Euler's equations for a deformable body are set up in an inertial (or fixed) coordinate system without any restriction on the stress tensor. Application of these equations is made for a simple viscous fluid body. Then, the Eulerian equations are formulated explicitly for three-dimensional rotation of self-gravitating compressible celestial bodies of arbitrary structure, and the viscosity of their material is treated as an arbitrary function of spatial coordinates, with special respect to a description of the effects of tidal deformation in a close pair of such bodies.
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Tokis, J.N. Rotational dynamics of deformable celestial bodies. Astrophys Space Sci 26, 447–476 (1974). https://doi.org/10.1007/BF00645625
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DOI: https://doi.org/10.1007/BF00645625