Abstract
Io is the most tidally heated world in the Solar System. In this chapter, we review the basics of how Io (and other satellites) responds to tidal forces, and how those forces shape Io’s interior structure and geologic activity. We also summarize the current state of knowledge of Io’s interior, largely gleaned from the Voyager and Galileo missions, along with ground and space-based observations. Despite decades of work, there are still many important, unanswered questions about tidal heating and the interior structure of Io, motivating continued research and exploration.
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Notes
- 1.
Co-latitude is the angular distance from the north pole: co-latitude = 90∘− latitude.
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Acknowledgements
The authors acknowledges substantial input from the Tidal Heating—Lessons from Io and the Jovian System workshop organized by the W.M. Keck Institute for Space Studies in 2018 (de Kleer et al. 2019b). A portion of this work was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). The authors thank Francis Nimmo for thoughtful edits which enhanced this chapter. Ⓒ 2022. All rights reserved.
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Keane, J.T., Matsuyama, I., Bierson, C.J., Trinh, A. (2023). Tidal Heating and the Interior Structure of Io. In: Lopes, R.M.C., de Kleer, K., Tuttle Keane, J. (eds) Io: A New View of Jupiter’s Moon . Astrophysics and Space Science Library, vol 468. Springer, Cham. https://doi.org/10.1007/978-3-031-25670-7_4
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