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The load of Tharsis has had both regional and global influences.<ref name="Golombek" /> Extensional features radiating from Tharsis include [[graben]] several kilometers wide, and hundreds of meters deep, as well as enormous troughs and rifts up to 600 km wide and several kilometers deep. These graben and rifts are bounded by steeply dipping [[normal fault]]s, and can extend for distances up to 4000 km. Their relief indicates that they accommodate small amounts of extension on the order of 100 m or less. It has been argued that these graben are surface expressions of deflated subsurface [[Dike (geology)|dikes]].<ref name="WilsonHead">{{cite journal|last1=Wilson|first1=L.|last2=Head III|first2=J. W.|title=Tharsis-Radial Graben Systems as the Surface Manifestation of Plume-Related Dike Intrusion Complexes: Models and Implications|journal=Journal of Geophysical Research: Planets|date=2002|volume=107|issue=E8|pages=5057–5080|doi=10.1029/2001JE001593|bibcode=2002JGRE..107.5057W|url=http://planetary.brown.edu/pdfs/2584.pdf}}</ref> |
The load of Tharsis has had both regional and global influences.<ref name="Golombek" /> Extensional features radiating from Tharsis include [[graben]] several kilometers wide, and hundreds of meters deep, as well as enormous troughs and rifts up to 600 km wide and several kilometers deep. These graben and rifts are bounded by steeply dipping [[normal fault]]s, and can extend for distances up to 4000 km. Their relief indicates that they accommodate small amounts of extension on the order of 100 m or less. It has been argued that these graben are surface expressions of deflated subsurface [[Dike (geology)|dikes]].<ref name="WilsonHead">{{cite journal|last1=Wilson|first1=L.|last2=Head III|first2=J. W.|title=Tharsis-Radial Graben Systems as the Surface Manifestation of Plume-Related Dike Intrusion Complexes: Models and Implications|journal=Journal of Geophysical Research: Planets|date=2002|volume=107|issue=E8|pages=5057–5080|doi=10.1029/2001JE001593|bibcode=2002JGRE..107.5057W|url=http://planetary.brown.edu/pdfs/2584.pdf}}</ref> |
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Circumferential to Tharsis are so-called [[wrinkle ridge]]s.<ref name="Golombek" /> These are compressional structures composed of linear asymmetric ridges that can be tens of kilometers wide and hundreds of kilometers long. Many aspects of these ridges appear to be consistent with terrestrial compressional features that involve surface folding overlying [[Thrust fault#Blind thrust faults|blind thrust faults]] at depth.<ref name="Schultz2000">{{cite journal|last1=Schultz|first1=R. A.|title=Localization of Bedding Plane Slip and Backthrust Faults Above Blind Thrust Faults: Keys to Wrinkle Ridge Structure|journal=Journal of Geophysical Research: Planets|date=2000|volume=105|issue=E5|pages=12035–12052|doi=10.1029/1999JE001212|bibcode=2000JGR...10512035S |
Circumferential to Tharsis are so-called [[wrinkle ridge]]s.<ref name="Golombek" /> These are compressional structures composed of linear asymmetric ridges that can be tens of kilometers wide and hundreds of kilometers long. Many aspects of these ridges appear to be consistent with terrestrial compressional features that involve surface folding overlying [[Thrust fault#Blind thrust faults|blind thrust faults]] at depth.<ref name="Schultz2000">{{cite journal|last1=Schultz|first1=R. A.|title=Localization of Bedding Plane Slip and Backthrust Faults Above Blind Thrust Faults: Keys to Wrinkle Ridge Structure|journal=Journal of Geophysical Research: Planets|date=2000|volume=105|issue=E5|pages=12035–12052|doi=10.1029/1999JE001212|bibcode=2000JGR...10512035S}}</ref> Wrinkle ridges are believed to accommodate small amounts of shortening on the order of 100 m or less. Larger ridges and scarps have also been identified on Mars. These features can be several kilometers high (as opposed to hundreds of meters high for wrinkle ridges), and are thought to represent large lithosphere-scale thrust faults.<ref name="TanakaSchultz">{{cite journal|last1=Tanaka|first1=K. L.|last2=Schultz|first2=R. A.|title=Lithospheric-Scale Buckling and Thrust Structures on Mars: The Coprates Rise and South Tharsis Ridge Belt|journal=Journal of Geophysical Research: Planets|date=1994|volume=99|issue=E4|pages=8371–8385|doi=10.1029/94JE00277|bibcode=1994JGR....99.8371S|url=https://zenodo.org/record/1231345}}</ref> Displacement ratios for these are ten times those of wrinkle ridges, with shortening estimated to be hundreds of meters to kilometers. |
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Approximately half of the extensional features on Mars formed during the Noachian, and have changed very little since, indicating that tectonic activity peaked early on and decreased with time. Wrinkle ridge formation both around Tharsis and in the eastern hemisphere is thought to have peaked in the [[Hesperian]], likely due to global contraction attributed to cooling of the planet.<ref name="Golombek" /> |
Approximately half of the extensional features on Mars formed during the Noachian, and have changed very little since, indicating that tectonic activity peaked early on and decreased with time. Wrinkle ridge formation both around Tharsis and in the eastern hemisphere is thought to have peaked in the [[Hesperian]], likely due to global contraction attributed to cooling of the planet.<ref name="Golombek" /> |
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