Galileo Regio: Difference between revisions
Cimon Avaro (talk | contribs) Uruk Sulcus to the south |
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{{Short description|Dark region on Callisto}} |
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{{infobox feature on Ganymede |
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{{Infobox feature on celestial object |
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|name=Galileo Regio |
|name = Galileo Regio |
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|image=[[Image:Ganymede g1 true.jpg|250px]] |
|image = [[Image:Ganymede g1 true 2.jpg|250px]] |
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|caption=The large dark oval region in the upper right is Galileo Regio |
|caption = The large dark oval region in the upper right is Galileo Regio |
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|latitude=47.0 |
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|coordinates = {{coord|47.0|N|129.6|W|globe:ganymede_type:landmark|display=inline,title}} |
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|N_or_S=N |
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|longitude=129.6 |
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|E_or_W=W |
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}} |
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'''Galileo Regio''' is a large |
'''Galileo Regio''' is a large, dark surface feature on Jupiter's moon [[Ganymede (moon)|Ganymede]].<ref name = "USGS_Galileo_Regio">{{cite web |
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| title = Galileo Regio |
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| work = Gazetteer of Planetary Nomenclature |
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| publisher = [[USGS Astrogeology Science Center]] |
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| url = http://planetarynames.wr.usgs.gov/Feature/2076 |
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| accessdate = 2015-05-16}}</ref> |
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It is a region of ancient dark material that has been broken apart by tectonism and is now surrounded by younger, brighter material (such as that of [[Uruk Sulcus]]) that has been upwelling from Ganymede's interior. It is thought to be some 4 billion years old and is heavily cratered and palimpsested, but also has a unique distribution of furrows and smooth terrain that has been the subject of conflicting speculation regarding cause or origin. The distribution of smooth terrain on Galileo Regio suggests that the ancient crust of Ganymede was relatively thin in the equatorial region and thickened poleward in this area. The age relationships, morphology, and geometry of the furrow systems do not favor an origin by impact or tidal stressing. A possible, but speculative, origin is crustal uplift caused by a plume-like convection cell in a fluid mantle underlying a thin crust. Stratigraphic and morphologic relationships among furrows and crater palimpsests suggest that palimpsest morphology is largely the result of impact into a rheologically weak crust rather than viscous relaxation. |
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Galileo Regio is bounded on the south by the [[Uruk Sulcus]] quadrangle. |
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The regio is bounded on the southwest by Uruk Sulcus, which lies between it and [[Marius Regio]]. Within Galileo Regio itself lies the [[Palimpsest (planetary astronomy)|palimpsest]] [[Memphis Facula]], a relic of an [[impact crater]] that has been flattened in a manner characteristic of some of the Solar System bodies with icy crusts. |
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{{astro-stub}} |
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==References== |
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{{reflist}} |
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# Harland, D. M.; Jupiter Odyssey, Springer Praxis (2000), p. 141 |
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# Casacchia, R., and R. G. Strom (1984), Geologic evolution of Galileo Regio, Ganymede, J. Geophys. Res., 89(S02), B419–B428, doi:10.1029/JB089iS02p0B419. |
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{{Ganymede}} |
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[[Category:Ganymede (moon)]] |
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Revision as of 10:06, 27 April 2024
 The large dark oval region in the upper right is Galileo Regio | |
| Feature type | Regio |
|---|---|
| Coordinates | 47°00′N 129°36′W / 47.0°N 129.6°W |
| Diameter | 3,200 km |
| Eponym | Galileo Galilei |
Galileo Regio is a large, dark surface feature on Jupiter's moon Ganymede.[1]
It is a region of ancient dark material that has been broken apart by tectonism and is now surrounded by younger, brighter material (such as that of Uruk Sulcus) that has been upwelling from Ganymede's interior. It is thought to be some 4 billion years old and is heavily cratered and palimpsested, but also has a unique distribution of furrows and smooth terrain that has been the subject of conflicting speculation regarding cause or origin. The distribution of smooth terrain on Galileo Regio suggests that the ancient crust of Ganymede was relatively thin in the equatorial region and thickened poleward in this area. The age relationships, morphology, and geometry of the furrow systems do not favor an origin by impact or tidal stressing. A possible, but speculative, origin is crustal uplift caused by a plume-like convection cell in a fluid mantle underlying a thin crust. Stratigraphic and morphologic relationships among furrows and crater palimpsests suggest that palimpsest morphology is largely the result of impact into a rheologically weak crust rather than viscous relaxation.
The regio is bounded on the southwest by Uruk Sulcus, which lies between it and Marius Regio. Within Galileo Regio itself lies the palimpsest Memphis Facula, a relic of an impact crater that has been flattened in a manner characteristic of some of the Solar System bodies with icy crusts.
References
- ^ "Galileo Regio". Gazetteer of Planetary Nomenclature. USGS Astrogeology Science Center. Retrieved 2015-05-16.
- Harland, D. M.; Jupiter Odyssey, Springer Praxis (2000), p. 141
- Casacchia, R., and R. G. Strom (1984), Geologic evolution of Galileo Regio, Ganymede, J. Geophys. Res., 89(S02), B419–B428, doi:10.1029/JB089iS02p0B419.
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