MARS THROUGH TIME
The Warm and Wet Climatic Phase of Early Mars: Geological and Hydrological Evidence from the Noachian to Early Hesperian Periods
The Noachian to early Hesperian epochs
represent a climatically significant period in Martian history, commonly referred to as the "Warm and Wet" phase. This interval is characterized by pervasive evidence of surface water activity and a sustained hydrologic cycle. Geologic indicators, including extensively developed valley networks, stratified sedimentary deposits, and aqueous alteration minerals such as phyllosilicates (clay minerals) and sulfates support the hypothesis that long-standing bodies of water were present during this time (Carr, 1996; Fassett & Head, 2008; Bibring et al., 2006) (Fig. 6). These may have included lacustrine environments and possibly shallow epeiric (epicontinental) seas.
Although Mars lacks Earth-like plate
Figure 6. A diagram originates from NASA’s Mars Science Laboratory (MSL) Curiosity Rover mission using Mstcam to study the chemical composition of the Knorr rock in the Gale Crater and strongly support water-related mineral formation such as kaolinite and gypsum (Grotzinger, J. P., et al., 2014).
tectonics, the planet experienced considerable tectonic deformation, particularly within the Tharsis region, due to active hot spots. This region exhibits a complex array of tectonic features, including
normal faults, grabens, folds, and rift systems, most prominently expressed in Valles Marineris, one of the largest known canyon systems in the solar system (Schultz & Watters, 2009). Tectonic and volcanic processes during this period also contributed to crustal formation, especially within the southern highlands (Figs. 7 and 8).
This period is interpreted as one of the most hydrologically active in Martian geological history, marked by sustained precipitation, surface runoff, subsurface infiltration, and the development of extensive fluvial networks. Geomorphologic features such as sinuous rilles, stream channels, gullies, alluvial fans, and deltaic deposits (Fig. 9), as well as large-scale dendritic drainage patterns, indicate widespread fluvial erosion and sediment transport (Fassett
Figure 7. A photograph of a twisted terrain in Hellas Planitia (actually located in Noachis quadrangle). Highly deformed area that records the early stage of Martian formation (Moore, J. M., Belton, M. J. S., & Goldsby, D. L., 1998).
its dynamo activity, leading to the loss of a global magnetic field (Acuna et al. 1999) (Fig. 5).
This cycle also marks the onset of the fundamental hydrological
systems on Mars. The extreme climatic regime during this interval was closely linked to intense meteoritic bombardment, widespread volcanism, and notable crustal deformation (Squyres and Carr 1986; Banerdt et al. 1992). These dynamic processes resulted in the formation of impact craters, tectonic structures such as folds, faults, and joints, as well as ridges and troughs, all indicative of a highly unstable and geologically active early Martian environment (Tanaka et al. 2014).
Figure 8. A photograph of a magnificent fault slip on Mars (white line) observed by the American Mars Reconnaissance Orbiter (NASA/JPL/ University of Arizona, 2007).
10 TPG •
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