Chavan, A., Bhore, V., Bhandari, S.
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2022.115118]
Department of Earth and Environmental Science, K.S.K.V. Kachchh University, Bhuj 370001, India
Copyright Elsevier

Martian geology and surface geomorphic features are grouped under Noachian, Hesperian, and Amazonian eras, based on the crater retention ages and resurfacing ages by crater densities. Comparing the similarities and differences between Martian landforms and their terrestrial analogues promotes an understanding of how surface processes operated on both planets. The study focusses on the processes responsible for the evolution of fluvial valleys flanking volcanic channels and the fluvial terraces with an objective towards ascertaining the role of changing climate, tectonic, and volcanic conditions. We have studied the channels that developed on the flank of volcanic crater Ceraunius Tholus and compared with the monogenetic volcanic field of Dhinodhar Hill which have been significantly modified by fluvial processes. Similarly, the fluvial basins developed on the Hesperian volcanic units of Euhus plateau were compared with the Alaldari drainage of Upper Tapi river basin, showing the development of theater-headed channels and valleys, and relative fluvial features showing the strong influence of catastrophic climate and tectonic, which is also supported by the morphometric analysis in modulating the topography. The fluvial terraces developed in the Nubra and Shyok rivers of Ladakh and Upper and Middle reaches of Sutlej in Central Himalayas are compared with Noctis fossae on Mars both developed due to the interplay of tectonism and climate.