Interiors of Earth-like planets and satellites of the solar system
Breuer, D.; Spohn, T.; Van Hoolst, T.; van Westrenen, W.; Stanley, S.; Rambaux, N. (2022). Interiors of Earth-like planets and satellites of the solar system. Surveys in Geophysics 43(1): 177-226. https://dx.doi.org/10.1007/s10712-021-09677-x In: Surveys in Geophysics. Kluwer Academic Publishers: Dordrecht; Tokyo; Lancaster; Boston. ISSN 0169-3298; e-ISSN 1573-0956, more Related to:Breuer, D.; Spohn, T.; Van Hoolst, T.; van Westrenen, W.; Stanley, S.; Rambaux, N. (2022). Correction to: Interiors of Earth-like planets and satellites of the solar system. Surveys in Geophysics 43(1): 227-228. https://dx.doi.org/10.1007/s10712-021-09687-9, more |  |
| Author keywords | Interior structure; Terrestrial planets and moons; Space exploration; Gravity; Rotation; Magnetic fields; Thermal evolution |
| Authors | | Top | - Breuer, D.
- Spohn, T.
- Van Hoolst, T., more
| - van Westrenen, W.
- Stanley, S.
- Rambaux, N., more
| |
| Abstract | The Earth-like planets and moons in our solar system have iron-rich cores, silicate mantles, and a basaltic crust. Differentiated icy moons can have a core and a mantle and an outer water-ice layer. Indirect evidence for several icy moons suggests that this ice is underlain by or includes a water-rich ocean. Similar processes are at work in the interiors of these planets and moons, including heat transport by conduction and convection, melting and volcanism, and magnetic field generation. There are significant differences in detail, though, in both bulk chemical compositions and relative volume of metal, rock and ice reservoirs. For example, the Moon has a small core [similar to 0.2 planetary radii (R-P)], whereas Mercury's is large (similar to 0.8 R-P). Planetary heat engines can operate in somewhat different ways affecting the evolution of the planetary bodies. Mercury and Ganymede have a present-day magnetic field while the core dynamo ceased to operate billions of years ago in the Moon and Mars. Planets and moons differ in tectonic style, from plate-tectonics on Earth to bodies having a stagnant outer lid and possibly solid-state convection underneath, with implications for their magmatic and atmosphere evolution. Knowledge about their deep interiors has improved considerably thanks to a multitude of planetary space missions but, in comparison with Earth, the data base is still limited. We describe methods (including experimental approaches and numerical modeling) and data (e.g., gravity field, rotational state, seismic signals, magnetic field, heat flux, and chemical compositions) used from missions and ground-based observations to explore the deep interiors, their dynamics and evolution and describe as examples Mercury, Venus, Moon, Mars, Ganymede and Enceladus. |
|
