Thaumasia Planum is a large volcanic highland plateau south of the deep canyons Melas and Coprates Chasma - two tectonic fault structures that are part of the vast, 4000-kilometre-long Valles Marineris valley system. The 'Plain of Thaumas' is named after a sea god in Greek mythology and consists largely of solidified lava flows.
These flows are up to several thousand metres thick, much thicker than anything found on the continents of Earth. The lava probably erupted during the Noachian period, the oldest of the three martian geological eras. It is therefore approximately four billion years old. Thaumasia is bordered on the east by a 900-kilometre-long ridge running north to south, informally referred to as Coprates Ridge.
The HRSC images presented here show the eastern flank of the Coprates Ridge, which contains tectonic fault structures of the Nectaris Fossae as well as the wide valleys of the dried-up Protva Valles river system. The topography indicates massive alteration of the landscape due to movements in the martian crust, which resulted in the formation of the tectonic grabens, and subsequent erosion. Some landforms are the result of outflowing lava that then solidified into a thin layer, creating what are referred to as wrinkled ridges.
Magma bubbles formed large parts of the martian crust
The formation of the Nectaris Fossae probably began in the Noachian era and possibly continued into the following martian age - the late Hesperian - when Mars increasingly took on its present shape. The grabens are thought to be 'genetically' linked to the Valles Marineris system, that is, they were formed by stretching of the crust due to uplift caused by rising magma bubbles. In this HRSC observation, the fissures cut almost straight through the image and are often filled with brightly coloured dust or sand.
The valley network of Protva Valles is heavily weathered by erosion. Its origin has been dated to the late Noachian and early Hesperian periods - a time when much more water flowed over the surface of Mars, carrying eroded material and reshaping the surface.
The development of the region may have begun with the uplift from the mass of the Tharsis volcanoes, which are up to 20 kilometres high, and the Olympus Mons megavolcano. This uplift may have caused stresses in the rock crust and led to numerous extensional fractures. Afterwards, the region was repeatedly covered by basalt lava flows, the most common volcanic rock on Earth as well, consisting of a thin layer of lava rich in iron and magnesium. During a later phase, the region was covered by volcanic ash and dust. Eventually, run-off water eroded valleys into the landscape.
Where did the water come from?
Some of the valleys appear to be cut deeper into the rock, others are more shallow and wider. They also seem to originate at different elevation levels - an indication of a lowering of the groundwater table if the rivers were fed by escaping groundwater. However, due to severe erosion, it is difficult to determine the origin of the water. The height differences within this image are an impressive 4500 metres. This is a scale that is only seen on Earth when considering the highest mountain ranges, the Andes and the Himalayas. However, since Protva Valles was probably formed 3.8 billion years ago, the geology has changed little.
Image processing
The images were created using data acquired by the High Resolution Stereo Camera (HRSC) on 23 May 2022 during Mars Express orbit 23,232. The ground resolution is approximately 23 metres per pixel and the image is centred at about 301 degrees east and 27 degrees south. The colour image was created using data acquired by the nadir channel, the field of view of which is aligned perpendicular to the surface of Mars, and the colour channels of the HRSC. The oblique perspective view was generated using a Digital Terrain Model (DTM) and data acquired by the nadir channel and colour channels of the HRSC.
The anaglyph image, which creates a three-dimensional impression of the landscape when viewed with red/blue or red/green glasses, was derived from data acquired by the nadir channel and one of the stereo channels. The colour-coded topographic view is based on a DTM of the region, from which the topography of the landscape can be derived. The reference body for the HRSC DTM is a Mars equipotential surface (Areoid).
HRSC is a camera experiment developed and operated by the German Aerospace Center (DLR). The systematic processing of the camera data was carried out at the DLR Institute of Planetary Research. Personnel in the Department of Planetary Sciences and Remote Sensing at the Freie Universitat Berlin used these data to create the image products shown here.
Related Links
Mars Express at ESA
Mars News and Information at MarsDaily.com
Lunar Dreams and more
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