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Rocky planets sketch

Rocky planets impression as a flat design sketch.

Rocky planets impression as a flat design sketch by Lucía Pérez Díaz.

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Venus space mission sketch

Venus space mission impression as a flat design sketch.

Venus space mission impression as a flat design sketch by Lucía Pérez Díaz.

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Earth from Moon sketch

Earth from the Moon impression as a flat design sketch.

Earth from the Moon impression as a flat design sketch by Lucía Pérez Díaz.

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Earth interior model

Simplified model of the Earth’s interior and its global dynamics featuring a solid inner and a fluid outer core, a viscous partially molten but not fluid mantle, and characteristic surface topography.

Simplified model of the Earth interior and its global dynamics featuring a solid inner and a fluid outer core, a viscous partially molten but not fluid mantle, with hot material rising from the core-mantle boundary in form of active mantle plumes and cold material, including oceanic surface plates, sinking back into the mantle in a process called subduction. The dynamics in the Earth interior crucially shapes the rocky surface of the planet, creating mountain ranges and deep-sea trenches.

  • Creator: Fabio Crameri
  • This version: 06.10.2021
  • License: Attribution-ShareAlike 4.0 International (CC BY-SA 4.0)
  • Specific citation: This graphic by Fabio Crameri adjusted from Crameri & Tackley (2016) is available via the open-access s-ink.org repository.
  • Related reference: Crameri, F., and P. J. Tackley (2016), Subduction initiation from a stagnant lid and global overturn: new insights from numerical models with a free surface, Progress in Earth and Planetary Science, 3(1), 1–19, doi:10.1186/s40645-016-0103-8
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Planetary interior

Comparison of suggested mantle convection in the Earth (mobile-lid mode) and Venus (inefficient short slab mode).

Comparison of suggested mantle convection in Earth and Venus. Mobile-lid mantle convection in the Earth involves most surface plates (dark brown), which are recycled by sinking back into the deep mantle, where large low shear-wave velocity provinces (LLSVPs) exist (whitish). The ongoing plate destruction causes a more heterogeneous mantle and a surface of variable age, with young and thin oceanic plates and old and thick continental plates that remain at the surface. Mantle plumes (light red) tend to occur far away from sinking plates. By contrast, the mode of mantle convection on Venus is suggested to consist of a nearly immobile, mostly stagnant lid, and only localised, short sinking plate portions that are formed by (and thus spatially coincide with) hot mantle upwelling (light red). The resulting surface deformation matches observations from coronae on Venus. The short sinking portions do not, in contrast to Earth, significantly move their tail ends at the surface, which explains the uniformly aged, relatively thick surface plate (dark brown).

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Paleo surface topography (globe animation)

Animation of the Earth’s surface topography through the Cenozoic time (66 – 0 Ma) on the globe.

Animation of the Earth’s surface topography through the Cenozoic time (66–0 Ma) on the globe. Shown is the Straume et al. (2020) paleogeography model. The Scientific colour map ‘oleron‘ is used to represent data accurately and to all readers.

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Earth topography (globe animation)

Animations of the Earth’s surface topography on the globe.

Animations of the Earth’s surface topography on the globe. Shown is GEBCO2019 (www.gebco.net) global relief model of Earth’s surface that integrates land topography and ocean bathymetry. The Scientific colour map ‘oleron‘ is used to represent data accurately and to all readers.

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Mercury topography (globe animation)

Globe animations of surface topography of the planet Mercury.

Globe animations of surface topography of the planet Mercury showing data (MESS-H-MDIS-5-DEM-ELEVATION-V1.0) derived from Messenger missions. The Scientific colour map ‘batlow‘ is used to represent data accurately and to all readers.

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Venus topography (globe animation)

Animations of Venusian surface topography on the globe.

Animations of Venusian surface topography on the globe. Shown is the Venus Magellan Global Topography 4641m (v2) representing the version 2 (1997 release) of the Global Topographic Data Record (GTDR-SINUS.3;2) available from https://astrogeology.usgs.gov/search/map/Venus/Magellan/RadarProperties/. The Scientific colour map ‘bilbao‘ is used to represent data accurately and to all readers.

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