Shalbatana vallis: The Mars Express mission of the European Space Agency has spotlighted Shalbatana Vallis, a vast Martian valley showing strong evidence of ancient water activity, volcanic processes, and geological transformation.
According to United News of Bangladesh, the valley, located near the Martian equator, stretches about 1,300 kilometers, approximately the length of Italy. The High Resolution Stereo Camera (HRSC) aboard the Mars Express spacecraft recently captured a new image of the valley's northern section as it winds across the planet's surface. This image is part of the ongoing research into Mars' geological past, which includes a video released in October 2025 tracing the valley's path from its source in the highlands of Xanthe Terra to its endpoint in the smoother terrain of Chryse Planitia.
Scientists believe that Shalbatana Vallis was formed around 3.5 billion years ago due to massive underground water bursts that carved deep channels as they flowed downhill. The main valley, approximately 10 kilometers wide and up to 500 meters deep, was likely deeper in the past, but sediment deposits have gradually filled parts of the channel over time. A notable dark patch in the rougher section of the valley is thought to be volcanic ash that was later redistributed by Martian winds.
Shalbatana Vallis is among many outflow channels marking the transition between Mars' heavily cratered southern highlands and the smoother northern lowlands. Near the valley lies Chryse Planitia, one of the planet's lowest regions, where many major outflow channels end. Scientists suggest that during a warmer and wetter period in Mars' history, this area might have hosted a large ocean.
The surrounding region of Shalbatana Vallis is characterized by 'chaotic terrain,' which includes broken rock blocks, ridges, and irregular landforms. This terrain likely formed when underground ice melted, causing the ground above to collapse. Similar features have been observed in other Martian areas, such as Pyrrhae Regio, Iani Chaos, Ariadnes Colles, Aram Chaos, and Hydraotes Chaos.
Numerous impact craters are visible across the region, with some remaining sharply defined while others appear partially buried or eroded. Several craters are surrounded by ejecta blankets, debris thrown outward during impacts. Parts of the terrain exhibit a smoother appearance, suggesting past lava flows. As the lava cooled and contracted, it formed wrinkle ridges. Additionally, isolated hills, or mesas, are visible as remnants of older elevated surfaces.
The HRSC camera is one of eight instruments aboard Mars Express, which has been studying Mars since its launch in 2003. Over more than two decades, the mission has significantly advanced the understanding of Mars' geological history, producing detailed color and three-dimensional maps of the planet. The camera was developed by the German Aerospace Center (DLR), and data is processed in Berlin and further analyzed by researchers at Freie Universit¤t Berlin.