Effect of tidal-heating on the rheology of Io
Allard K. Veenstra (TU Delft - Planetary Exploration)
Teresa Steinke (TU Delft - Astrodynamics & Space Missions)
M. Rovira-Navarro (TU Delft - Planetary Exploration)
Wouter van der Wal (TU Delft - Planetary Exploration)
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Abstract
Io exhibits widespread volcanism powered by tides raised by Jupiter. The distribution of volcanoes offers a window into the interior of the moon. The distribution shows more volcanism at the equator as well as peak volcanic output which is shifted by roughly 30-60 degrees to the east of the subjovian point [1]. Models of tidal dissipation that assume a spherically symmetric, solid Io cannot reproduce this shift [2]. More recently, it has been proposed that tidal dissipation in a magma ocean [3] or in a non-spherically symmetric, solid Io [4] can induce this lag. In this study, we explore the second option and show that solid-body dissipation can induce an eastward shift of the tidal dissipation pattern.
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