Topography Of Mars
Abstract: The environment of Mars is controlled by a myriad of processes, however water and weathering on the surface of Mars is still an extremely controversial topic. This project aims to explore the current evidence we have for liquid water in the past and present by inspecting the geomorphological evidence and evaluate the role it plays in shaping Mars’ topography. From terrestrial analogs, we can begin to explain the processes that occur on Mars. Due to the similarities of outflow channels, valley network and gullies to its terrestrial counterparts, we have suspected that these landforms are carved by water. Further evidence of water on Mars are evapourite deposits and fan deposits found near valley networks. However, there are major
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It appears as though Mars runs on the many processes that are similar to earth. The interplay of air, water, ice and geology create and control the environment on Mars. By applying our knowledge of earth’s processes along with physical modeling, we can begin to also explain these processes that occur on Mars (Head 2007). Impact craters characterize the first-order topography and modify the Martian surface through vertical excavation and transportation of crustal material (Head 2007). Moreover, evidence of volcanism is abundant. Lava flows can form channels, valleys networks and smooth plains, and there are many extinct volcanoes, the largest volcano in the solar system Mount Olympus is found on Mars. There is also some evidence for tectonic activity on Mars shown through the structural features such as rifts, trough and ridges, however evidence is minimal and remains a controversial topic (Head 2007). Despite having a thin atmosphere, wind processes are still supported on Mars’ atmosphere. Aeolian processes currently dominate the surface, creating and shaping the present day landform as volcanic, tectonic and water activity on Mars appears to be inactive currently (Head
It appears as though Mars runs on the many processes that are similar to earth. The interplay of air, water, ice and geology create and control the environment on Mars. By applying our knowledge of earth’s processes along with physical modeling, we can begin to also explain these processes that occur on Mars (Head 2007). Impact craters characterize the first-order topography and modify the Martian surface through vertical excavation and transportation of crustal material (Head 2007). Moreover, evidence of volcanism is abundant. Lava flows can form channels, valleys networks and smooth plains, and there are many extinct volcanoes, the largest volcano in the solar system Mount Olympus is found on Mars. There is also some evidence for tectonic activity on Mars shown through the structural features such as rifts, trough and ridges, however evidence is minimal and remains a controversial topic (Head 2007). Despite having a thin atmosphere, wind processes are still supported on Mars’ atmosphere. Aeolian processes currently dominate the surface, creating and shaping the present day landform as volcanic, tectonic and water activity on Mars appears to be inactive currently (Head