The rotation of Venus. Part 1: Atmospheric tides. Part 2: Obliquity and evolution

Details The rotation of Venus. Part 1: Atmospheric tides. Part 2: Obliquity and evolution The rotation of Venus. Part 1: Atmospheric tides. Part 2: Obliquity and evolution

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979phdt.........2d&link_type=abstract

Ph.D. Thesis California Inst. of Tech., Pasadena.

Other

Atmospheric Tides, Planetary Evolution, Planetary Rotation, Venus (Planet), Oblique Coordinates, Planetary Surfaces, Quantitative Analysis, Tides

Scientific paper

Earth-based radar-observations reveal that the surface of Venus rotates very slowly in the retrograde sense. Tides raised by the sun in the body of Venus tend to slow its rotation further. The spin of Venus might be in a steady state if thermal tides in the atmosphere balance the tidal torque on the crust. Part 1 of this dissertation presents a quantitative theory of atmospheric tides applicable to Venus. It is found that the thermal tide is capable of maintaining the rotation of Venus in its current state indefinitely. Part 2 examines the effects of obliquity, the frequency-dependence of the tides, core-mantle coupling, possible resonances, and other phenomena. It appears most likely that Venus originated with an obliquity greater than 90 deg.

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