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Breuer, Doris [Author]; Spohn, Tilman [Author]; Van Hoolst, Tim [Author]; van Westrenen, Wim [Author]; Stanley, Sabine [Author]; Rambaux, Nicolas [Author]; DLR Institut für Planetenforschung, Berlin, Germany [Author]; Institute of Astronomy, KU Leuven, Leuven, Belgium [Author]; Vrije Universiteit Amsterdam, Amsterdam, The Netherlands [Author]; Department of Erath and Planetary Sciences, John Hopkins University, Baltimore, MD, USA [Author]; Institut de Mécanique Céleste et des Ephémérides, Observatoire de Paris, CNRS, PSL Research University, Sorbonne Université, Université de Lille, Paris, France [Author]

Interiors of Earth-Like Planets and Satellites of the Solar System

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  • Media type: E-Article
  • Title: Interiors of Earth-Like Planets and Satellites of the Solar System
  • Contributor: Breuer, Doris [Author]; Spohn, Tilman [Author]; Van Hoolst, Tim [Author]; van Westrenen, Wim [Author]; Stanley, Sabine [Author]; Rambaux, Nicolas [Author]; DLR Institut für Planetenforschung, Berlin, Germany [Author]; Institute of Astronomy, KU Leuven, Leuven, Belgium [Author]; Vrije Universiteit Amsterdam, Amsterdam, The Netherlands [Author]; Department of Erath and Planetary Sciences, John Hopkins University, Baltimore, MD, USA [Author]; Institut de Mécanique Céleste et des Ephémérides, Observatoire de Paris, CNRS, PSL Research University, Sorbonne Université, Université de Lille, Paris, France [Author]
  • imprint: Springer Netherlands, 2021-12-14
  • Language: English
  • DOI: https://doi.org/10.1007/s10712-021-09677-x
  • Keywords: Gravity ; Thermal evolution ; Interior structure ; Space exploration ; Terrestrial planets and moons ; Rotation ; Magnetic fields
  • Origination:
  • Footnote: Diese Datenquelle enthält auch Bestandsnachweise, die nicht zu einem Volltext führen.
  • Description: 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 [~ 0.2 planetary radii (RP)], whereas Mercury’s is large (~ 0.8 RP). 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. ; Deutsches Zentrum für Luft- und Raumfahrt e. V. (DLR) (4202)
  • Access State: Open Access
  • Rights information: Attribution (CC BY)