Pluto and Triton: Interactions Between Volatiles and Dynamics

Details Pluto and Triton: Interactions Between Volatiles and Dynamics Pluto and Triton: Interactions Between Volatiles and Dynamics

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaop.work...75r&link_type=abstract

Forum on Innovative Approaches to Outer Planetary Exploration 2001-2020, p. 75

Statistics

Polar Caps, Tides, Triton, Polar Wandering (Geology), Pluto (Planet), Neptune (Planet), Charon, Precession

Scientific paper

Volatiles moving across the surfaces of Pluto and Triton can give rise to interesting dynamical consequences. Conversely, measurement of dynamical states can help constrain the movement of volatiles and interior structure of both bodies. Polar wander may theoretically occur on both Triton and Pluto. Triton's obliquity is low, so that the equatorial regions receive more insolation than the poles. Hence there is a tendency for nitrogen ice to sublime at the equator and condense at the poles, creating polar caps. If the nitrogen supply is large enough, then these caps could move in approximately 105 years the global equivalent of 200 m of ice to the poles. At this point the equatorial moment of inertia becomes larger than the moment of inertia measured about the rotation axis, so that Triton overbalances and becomes dynamically unstable. The satellite then undergoes polar wander, restoring stability when the new equator contains the excess matter. Hence the pole may be continually wandering. Neptune raises a permanent tidal bulge on Triton, so that the satellite's surface is elongated like a football, with the long axis pointing at Neptune. This is expected to be the axis about which the pole wanders. Volatile migration would resurface the satellite to some depth and wandering would disturb leading side/trailing side crater statistics. Additional information is contained in the original extended abstract.

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