Abstract
Possible orientations of the Venus rotation pole as a function of planetary oblateness are calculated, taking into account the variation of the orbital inclination and motion of the nodal line produced by long-term planetary perturbations and assuming the obliquity to be fully damped. If the obliquity is stabilized against solar tides by core-mantle viscous coupling, a fully damped obliquity is the expected state. An analysis of earth-based radar data from 1964 to 1977 yields a pole position which lies near damped pole positions of small oblateness, no more than about 10 to the 6th. Possible implications of this result are considered.
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