Atmospheric tides and the rotation of Venus. II - Spin evolution

Details Atmospheric tides and the rotation of Venus. II - Spin evolution Atmospheric tides and the rotation of Venus. II - Spin evolution

Jan 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...41...18d&link_type=abstract

Icarus, vol. 41, Jan. 1980, p. 18-35.

Mathematics

19

Atmospheric Tides, Planetary Rotation, Spin Dynamics, Venus Atmosphere, Angular Momentum, Nutation, Precession, Solar Gravitation, Venus, Rotation, Atmosphere, Tidal Forces, Torque, Surface, Absorption, Heating, Circulation, Crust, Spin, Friction, Cores, Gravitational Fields, Mantle, Mathematical Models, Viscosity, Data, Evolution, Nutation, Precession, Resonance, Dynamics, Obliquity, Equations Of Motion, Temperatures, Pressure, Winds

Scientific paper

Tides in the atmosphere of Venus may help to stabilize its slow retrograde rotation. The frequency dependence of the body tides also affects its rotational stability. However, the obliquity is probably maintained near 180 deg by friction between the core and mantle of Venus. In any case, it appears most likely that Venus originated with an obliquity greater than 90 deg.

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