Linear ridge networks

Linear ridge networks are found in various places on Mars in and around craters.^[1] Ridges often appear as mostly straight segments that intersect in a lattice-like manner. They are hundreds of meters long, tens of meters high, and several meters wide. It is thought that impacts created fractures in the surface, these fractures later acted as channels for fluids. Fluids cemented the structures. With the passage of time, surrounding material was eroded away, thereby leaving hard ridges behind. It is reasonable to think that on Mars impacts broke the ground with cracks since faults are often formed in impact craters on Earth. One could guess that these ridge networks were dikes, but dikes would go more or less in the same direction, as compared to these ridges that have a large variety of orientations. Since the ridges occur in locations with clay, these formations could serve as a marker for clay which requires water for its formation.^[2]^[3]^[4] Water here could have supported past life in these locations. Clay may also preserve fossils or other traces of past life. These ridges could be formed by large impacts that produced fractures, faults, or dikes made up of melted rock and/or crushed rock (breccia). If the impact-caused dike is made of purely melted rock from the heat of the impact, it is called a pseudotachylite .^[5] Also, hydrothermalism may have been involved. Because they seem to be found in older crust only, it is believed that they occurred early in the history of Mars when there were more and larger asteroids striking the planet. These early impacts may have caused the early crust to be full of interconnected channels.^[6]^[7] These networks have been found many regions of Mars including in Arabia Terra (Arabia quadrangle), northern Meridiani Planum, Solis Planum, Noachis Terra (Noachis quadrangle), Atlantis Chaos, and Nepenthes Mensa (Mare Tyrrhenum quadrangle).^[8]

Linear ridge networks in Casius quadrangle

Network of ridges, as seen by HiRISE under HiWish program Ridges may be formed in various ways.
Color, close-up of ridges seen in previous image, as seen by HiRISE under HiWish program
More ridges from the same place as the previous two images, as seen by HiRISE under HiWish program
Linear ridge network, as seen by HiRISE under HiWish program
Close-up and color image of previous image of linear ridge network, as seen by HiRISe under HiWish program
More linear ridge networks from same location as previous two images, as seen by HiRISE under HiWish program

Linear ridge networks in Syrtis Major quadrangle

Huo Hsing Vallis in Syrtis Major, as seen by THEMIS. Straight ridges may be dikes in which liquid rock once flowed.
Huo Hsing Vallis Ridges, as seen by HiRISE. Ridges may be caused by water moving along faults.
Ridges, as seen by HiRISE under HiWish program These may be the result of dikes or faults.

Linear ridge networks in Phaethontis quadrangle

Linear ridge networks, as seen by HiRISE under HiWish program
Close-up of linear ridge networks from the previous image, as seen by HiRISE under HiWish program
Linear ridge networks, as seen by HiRISE under HiWish program
Linear ridge networks, as seen by HiRISE under HiWish program

Linear ridge networks in Amazonis quadrangle

Narrow ridges, as seen by HiRISE under HiWish program. The ridges may be the result of impacts fracturing the surface.
Linear ridge networks, as seen by HiRISE under HiWish program
Close-up of ridge network, as seen by HiRISE under HiWish program This is an enlargement of a previous image.
Close-up of ridge network, as seen by HiRISE under HiWish program This is an enlargement of a previous image.
Linear ridge networks, as seen by HiRISE under HiWish program

Linear ridge networks in Arabia quadrangle

Linear ridge network, as seen by HiRISE under HiWish program Dark line is not part of the picture.
Dikes in Arabia, as seen by HiRISE, under the HiWish program. These straight features may indicate where valuable ore deposits may be found by future colonists. Scale bar is 500 meters. They may be part of linear ridges, hence related to impact craters.
Close-up of a complex group of ridges. The ridges may be the remains of old streams and/or linear ridge networks. Image taken by HiRISE under the HiWish program.

Linear ridge networks in Mare Tyrrhenum quadrangle

Linear ridge network, as seen by HiRISE under HiWish program

References

↑ Head, J., J. Mustard. 2006. Breccia dikes and crater-related faults in impact craters on Mars: Erosion and exposure on the floor of a crater 75 km in diameter at the dichotomy boundary, Meteorit. Planet Science: 41, 1675-1690.
↑ Mangold et al. 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 2. Aqueous alteration of the crust. J. Geophys. Res., 112, doi:10.1029/2006JE002835.
↑ Mustard et al., 2007. Mineralogy of the Nili Fossae region with OMEGA/Mars Express data: 1. Ancient impact melt in the Isidis Basin and implications for the transition from the Noachian to Hesperian, J. Geophys. Res., 112.
↑ Mustard et al., 2009. Composition, Morphology, and Stratigraphy of Noachian Crust around the Isidis Basin, J. Geophys. Res., 114, doi:10.1029/2009JE003349.
↑ http://www.impact-structures.com/impact-rocks-impactites/the-impact-breccia-page/suevite-or-suevite-breccia-2/
↑ Ehlmann, G. et al. 2011. Subsurface water and clay mineral formation during the early history of Mars. Nature: 479, 53-61.
↑ E. K. Ebinger E., J. Mustard. 2015. LINEAR RIDGES IN THE NILOSYRTIS REGION OF MARS: IMPLICATIONS FOR SUBSURFACE FLUID FLOW. 46th Lunar and Planetary Science Conference (2015) 2034.pdf
↑ Saper, L., J. Mustard. 2013. Extensive linear ridge networks in Nili Fossae and Nilosyrtis, Mars: implications for fluid flow in the ancient crust. Geophysical Research letters: 40, 245-249.

This article is issued from Wikipedia - version of the Friday, April 08, 2016. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.