Ius and Tithonium Chasmata on Mars. This image from ESAs Mars Express reveals Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. This image from ESAs Mars Express reveals Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. The location outlined by the vibrant white box shows the location imaged by the Mars Express High Resolution Stereo Camera on April 21, 2022, throughout orbit 23123. This oblique viewpoint view of Tithonium Chasmata, which forms part of Mars Valles Marineris canyon structure, was generated from the digital surface model and the nadir and color channels of the High Resolution Stereo Camera on ESAs Mars Express.
The image at the top of this post reveals two trenches (or chasma) that form part of western Valles Marineris. Left wing (south), is the 840 km-long (522 mile-long) Ius Chasma, and on the right (north) is the 805 km-long (500 mile-long) Tithonium Chasma. Whilst these high-resolution images reveal amazing surface area information, it is only when we look at an elevation map that we recognize how incredibly deep the chasmata are– up to 7 km (4 miles)! At 4809 meters (15,777 feet), the Alps tallest mountain Mont Blanc would be overshadowed if it was put inside Tithonium Chasma.
Perspective view of Tithonium Chasma. This oblique perspective view of Tithonium Chasmata, which forms part of Mars Valles Marineris canyon structure, was produced from the digital surface model and the nadir and color channels of the High Resolution Stereo Camera on ESAs Mars Express. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
At the top of Tithonium Chasma, a spot of dark sand brings color contrast to the image. This sand might have come from the close-by Tharsis volcanic area.
Next to the dark sand dunes are 2 light-toned mounds (one cut in half by the upper image border). These mounds are more like mountains, increasing more than 3000 meters (10,000 feet) in height. Their surfaces have been highly worn down by Mars strong winds, showing that they are made of a weaker product than the surrounding rock.
Viewpoint view of Tithonium Chasma. This oblique viewpoint view of Tithonium Chasmata, which forms part of Mars Valles Marineris canyon structure, was created from the digital terrain design and the nadir and color channels of the High Resolution Stereo Camera on ESAs Mars Express. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
In between the two mounds we see a series of smaller bumps, as displayed in the 2nd viewpoint view. Examinations by Mars Express have actually discovered water-bearing sulfate minerals in this area. This recommends that these bumps may have formed when liquid that as soon as filled the chasma vaporized, although this theory is still fiercely discussed.
Topography of Ius and Tithonium Chasmata. This color-coded topographic image reveals Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. It was produced from data collected by ESAs Mars Express on April 21, 2022.
To the lower right of the mound that we see fully (upper right in the second perspective view), we can see parallel lines and particles piles that suggest a current landslide. This is likewise noticeable as a big purple location in the topography image below. The landslide was brought on by the collapse of the canyon wall on the right, and is likely to have actually happened reasonably just recently due to the fact that it has not been strongly deteriorated.
The gnarly flooring of Ius Chasma is equally remarkable. As tectonic plates pulled apart, they appear to have triggered jagged triangles of rock to form that appear like a row of shark teeth. With time, these rock developments have collapsed and eroded.
Ius and Tithonium Chasmata in 3D. This stereoscopic image shows Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. It was generated from information recorded by the High Resolution Stereo Camera (HRSC) on ESAs Mars Express on April 21, 2022, during orbit 23123. The anaglyph, originated from data gotten by the nadir channel and one stereo channel of the HRSC, offers a three-dimensional view when seen using red-blue or red-green glasses. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
Exploring Mars
Mars Express has been orbiting the Red Planet given that 2003, imaging Mars surface area, mapping its minerals, determining the structure and circulation of its tenuous environment, probing underneath its crust, and exploring how numerous phenomena interact in the martian environment.
The missions High Resolution Stereo Camera (HRSC), responsible for these new images, has revealed much about Mars diverse surface features, with recent images showing whatever from brain surface and wind-sculpted ridges and grooves through monstrous “claw mark” scratches to volcanoes, tectonic faults, river channels, and ancient lava swimming pools.
Ius and Tithonium Chasmata on Mars. This image from ESAs Mars Express shows Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. This image makes up data gathered by Mars Express High Resolution Stereo Camera (HRSC) on April 21, 2022. Credit: ESA/DLR/FU Berlin, CC BY-SA 3.0 IGO
ESAs Mars Expresss newest image release takes us over two ruptures in the martian crust that form part of the magnificent Valles Marineris canyon system.
Valles Marineris cuts throughout Mars comparable to how the Grand Canyon crosses the United States, other than the latter is tiny in contrast. At 4000 km (2500 miles) long, 200 km (125 miles) wide and up to 7 km (4 miles) deep, Valles Marineris is incredible. It is almost 10 times longer, 20 times wider, and five times deeper than the Grand Canyon. As the largest canyon system in our Solar System, it would cover the distance from the northern pointer of Norway to the southern suggestion of Sicily.
Ius and Tithonium Chasmata in context. This image from ESAs Mars Express reveals Ius and Tithonium Chasmata, which form part of Mars Valles Marineris canyon structure. The location outlined by the bold white box indicates the location imaged by the Mars Express High Resolution Stereo Camera on April 21, 2022, throughout orbit 23123. Credit: NASA/MGS/MOLA Science Team
Theres another substantial distinction in between the two: while the Grand Canyon was created as a result of rock being deteriorated by the Colorado River, Valles Marineris is believed to have actually formed through the drifting apart of tectonic plates.
