Physics
Scientific paper
May 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icar..163...24c&link_type=abstract
Icarus, Volume 163, Issue 1, p. 24-45.
Physics
24
Scientific paper
We present here the numerical application of the theoretical results derived in , Icarus 163, 1-23) for the spin evolution of Venus since its formation. We explore a large variety of initial conditions to cover the possible formation and evolutionary scenarios. In particular, we pay special attention to the evolutions which cross the chaotic zone resulting from secular planetary perturbations , Nature 361, 608-612). We demonstrate that Venus' axis can be temporarily trapped in a secular resonance with the node of Neptune's orbit, which can prevent it from being tilted to 180° and will drive it toward 0°. We test several dissipation models and parameters to evaluate their contribution to the planet's spin history. We confirm that despite the variations in the models, only three of the four final spin states of Venus are possible , Nature 411, 767-770) and that the present observed retrograde spin state of Venus can be attained by two different processes. In the first scenario (Fπ-), the axis is tilted toward 180° while its rotation rate slows down, while in the second one, the axis is driven toward 0° obliquity and the rotation rate decreases, stops, and increases again in the reverse direction to a final equilibrium value (F0-).
Correia Alexandre C. M.
Laskar Jacques
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