Relationships Between Wrinkle Ridges and Craters in Hesperia Planum: Constraints on the Timing of Ridge Formation

Details Relationships Between Wrinkle Ridges and Craters in Hesperia Planum: Constraints on the Timing of Ridge Formation Relationships Between Wrinkle Ridges and Craters in Hesperia Planum: Constraints on the Timing of Ridge Formation

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996lpi....27..869m&link_type=abstract

Lunar and Planetary Science, volume 27, page 869

Other

Hellas, Hesperia Planum, Mars, Tectonism, Wrinkle Ridges

Scientific paper

Wrinkle ridges in Hesperia Planum are similar in morphology to those in other regions of Mars such as Lunae Planum, the Coprates region, and Chryse Planitia and to lunar mare ridges. Martian wrinkle ridges have been classified into four types: high- and low-relief ridges, ridge rings, and rectilinear ridges. High- and low-relief ridges and ridge rings are believed to be compressional tectonic features formed in volcanic plains, whereas rectilinear ridges are thought to result from differential erosion or are the surface expressions of dikes.

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