Equations of motion for rotating finite bodies in the extended PPN formalism

Details Equations of motion for rotating finite bodies in the extended PPN formalism Equations of motion for rotating finite bodies in the extended PPN formalism

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977cemec..15..111d&link_type=abstract

Celestial Mechanics, vol. 15, Feb. 1977, p. 111-123.

Physics

6

Equations Of Motion, Gravitation Theory, Gravitational Effects, Relativity, Rotating Bodies, Rotating Fluids, Acceleration (Physics), Astronomical Models, Ideal Fluids, Instrument Errors, Laser Range Finders, Radio Range, Relativistic Velocity, Solar System, Space-Time Functions

Scientific paper

The equations of motion for rotating finite bodies are computed in the perfect fluid metric in the extended parametric post-Newtonian (PPN) formalism of Will and Nordtvedt (1972) and are used to build a model of the solar system consisting of N oblate, homogeneous, stationary, self-gravitating masses of rotating perfect fluid. These equations contain relativistic acceleration terms which are currently observable or may be observable in the future with improved radio and laser ranging techniques.

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