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This image from ESA’s Mars Express shows Nectaris Fossae and Protva Valles, complex geological features found on Mars. Round impact craters are scattered across the frame, and a band of fractured grooves, resembling scratches and scars carved into the rock, stretches from the top left to bottom right.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
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This image from ESA’s Mars Express shows Nectaris Fossae and Protva Valles, complex geological features found on Mars. Round impact craters are scattered across the frame, and a band of fractured grooves, resembling scratches and scars carved into the rock, stretches from the top left to bottom right.
Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
Mars displays fascinating geology everywhere you look—and nowhere is this more true than in the fractured, wrinkled ground seen in this image from ESA's Mars Express.
The scene, captured by the High Resolution Stereo Camera (HRSC) on the Mars Express orbiter, features the flanks of a vast volcanic plateau named Thaumasia Planum. The highest features visible here are a whopping 4500 m taller than the lowest, as seen most clearly in the associated topographical map. Many thought to have changed very little since they formed nearly four billion years ago, giving an exciting glimpse into Mars' earliest days.
Shifting plates
This complex region appears to have been shaped by both tectonics (deformation of the planetary crust) and by past running water.
While Mars no longer displays signs of active tectonics, this has not always been the case.
Mars' crust once experienced significant stresses in this region, creating the deep surface fractures today known as Nectaris Fossae. These are visible as near-vertical scars at the center of this image and have since been filled by light-colored dust. They are thought to have formed in relation to the colossal Valles Marineris canyon system, the largest such system not only on Mars but in the Solar System. Valles Marineris lies just to the north (right) of this region.
This oblique perspective view of Nectaris Fossae and Protva Valles on Mars was generated from the digital terrain model and the nadir and colour channels of the High Resolution Stereo Camera on ESA’s Mars Express. A large impact crater features in the bottom left, stretching partially out of frame, with four smaller craters dotted across to its right. Some textures and grooves can be seen in the more distant surface. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
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This oblique perspective view of Nectaris Fossae and Protva Valles on Mars was generated from the digital terrain model and the nadir and colour channels of the High Resolution Stereo Camera on ESA’s Mars Express. A large impact crater features in the bottom left, stretching partially out of frame, with four smaller craters dotted across to its right. Some textures and grooves can be seen in the more distant surface. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
Flowing water
After tectonism reworked this patch of Mars, water flowed across the surface, cutting into the rock and carving out deep valleys as it did so (features named Protva Valles—the plural 'Valles' referring to multiple channels). These channels can be seen spread across these images; some are broad and superficial and some far deeper. The dense patch of water-carved valleys to the bottom right of the image is intensely eroded.
Protva Valles formed when water was far more plentiful across the surface of Mars, some 3.8 billion years ago, and has remained largely unchanged since.
This image from ESA’s Mars Express shows Nectaris Fossae and Protva Valles on Mars. The area outlined by the bold white box indicates the area imaged by the Mars Express High Resolution Stereo Camera on 23 May 2022 during orbit 23232. Credit: NASA/MGS/MOLA Science Team
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This image from ESA’s Mars Express shows Nectaris Fossae and Protva Valles on Mars. The area outlined by the bold white box indicates the area imaged by the Mars Express High Resolution Stereo Camera on 23 May 2022 during orbit 23232. Credit: NASA/MGS/MOLA Science Team
Built on lava
The underlying terrain here—Thaumasia Planum—formed in the very earliest days of Mars and is largely made up of immense lava flows several kilometers thick.
This time was a turbulent one, with many of Mars' standout features just beginning to form. The Tharsis volcanoes, some of the largest in the Solar System, are located near to Thaumasia Planum; the load and stress of these volcanoes forming may have prompted this region to begin fracturing, before these volcanoes then flooded the area with lava.
Topography of Nectaris Fossae and Protva Valles. This color-coded topographic image shows Nectaris Fossae and Protva Valles on Mars. It was created from data collected by ESA’s Mars Express on 23 May 2022. It is based on a digital terrain model of the region, from which the topography of the landscape can be derived. Lower parts of the surface are shown in blues and purples, while higher altitude regions show up in whites and reds, as indicated on the scale to the top right. North is to the right. The ground resolution is approximately 23 m/pixel and the image is centered at about 27°S/301°E. Credit: European Space Agency
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Topography of Nectaris Fossae and Protva Valles. This color-coded topographic image shows Nectaris Fossae and Protva Valles on Mars. It was created from data collected by ESA’s Mars Express on 23 May 2022. It is based on a digital terrain model of the region, from which the topography of the landscape can be derived. Lower parts of the surface are shown in blues and purples, while higher altitude regions show up in whites and reds, as indicated on the scale to the top right. North is to the right. The ground resolution is approximately 23 m/pixel and the image is centered at about 27°S/301°E. Credit: European Space Agency
As these lava flows cooled and solidified on unstable, shifting ground, they became compressed, resulting in 'wrinkle ridges'. One of the most substantial ridges is seen to the bottom-right of center as an unsteady diagonal line scored into the surface.
Following this extensive resurfacing by lava, Thaumasia Planum was covered in volcanic ash and dust, before the water flows cut through the lava to form the Protva Valles. The origin of these water flows remains unclear; they appear to emerge at different heights, implying that water may have seeped through subsurface layers of Mars.