Timing and formation of wrinkle ridges in the Tyrrhena Patera Region of Mars

Details Timing and formation of wrinkle ridges in the Tyrrhena Patera Region of Mars Timing and formation of wrinkle ridges in the Tyrrhena Patera Region of Mars

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept...65p&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 65-66 (SEE N92-10728 01-91)

Physics

Geophysics

Calderas, Landforms, Mars Surface, Mars Volcanoes, Planetary Surfaces, Chronology, Fluid Flow, Lava, Mercury (Planet), Moon, Plains, Planetary Evolution

Scientific paper

Wrinkle ridges are distinctive linear to curvilinear arches topped by crenulated ridges and have been identified on the Moon, Mercury, and Mars. The presence of wrinkle ridges on other planetary surfaces has been used as a criterion for identifying volcanic plains. Recently, due to the presence of lava flow lobes and leveed channels, Greeley and Crown identified an area within Hesperia Planum as a flank flow unit associated with Tyrrhena Patera. Hesperia Planum surrounds Tyrrhena Patera and embays the eroded shield of the volcano to the north and south. The Tyrrhena Patera flank flow unit extends approx. 1000 km from the summit caldera to the southwest. More than 55 wrinkle ridges have been identified on this flank flow unit. The relationships between the lava flows and wrinkle ridges within the flank flow unit allow relative ages to be determined. Wrinkle ridges are classified as post flow if flow lobes appear to arch over the rises undeformed, with no evidence of flow ponding on the upstream side of the ridge, or of flows breaching the rises. Wrinkle ridges within Hesperia Planum and Tyrrhena Patera flank flow unit that trend NW-SE appear younger than the flank flow unit.

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