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However, other modeling studies find that the fluidization is unrelated to water and could be due to increased fragmentation ( Rager et al., 2014) or the presence of an erodible surface ( Wada and Barnouin-Jha, 2006)-yet both require preconditioning of the surface by water or water ice to explain the latitudinal distribution. Numerical models generally find this morphology to be consistent with either melting or a volatile-rich layer ( Baratoux et al., 2002 Oberbeck, 2009 Weiss and Head, 2014, 2013). Lobate ejecta morphologies (e.g., multilayer ejecta, double-layer ejecta- Fig. 9.14B) are interpreted to be the result of fluidization and are observed almost exclusively at the mid- to high-latitudes ( Barlow, 2006, 2005 Barlow and Perez, 2003 Costard, 1989 Mouginis-Mark, 1981, 1979).
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Image credits: NASA/JPL/MSSS/ESA/DLR/UofA. (F) Mojave Crater with alluvial fans on the inner craters slopes. Top THEMIS day IR-controlled mosaic image from the USGS and bottom HiRISE image ESP_016985_2315. (E) Lyot Crater with clastic polygonal networks in the ejecta. (D) Hale Crater with channels incising the ejecta. (C) Multilayer ejecta crater in southern hemisphere with channels incised into its ejecta blanket ( Mangold, 2012). (B) Double-layered ejecta crater in northern plains, with lobate margins and radiating grooves ( Weiss and Head, 2014). (A) Pits on the floor of <10 Ma Tooting Crater ( Mouginis-Mark and Boyce, 2012). Crater-related liquid water morphologies. Clastic polygonal networks in the ejecta of Lyot Crater ( Fig. 9.14E) even suggest that water in the ejecta blanket could result in longer term ice-segregation processes ( Brooker et al., 2018) and conical landforms in the ejecta flows at Hale Crater may also be suggestive of longer term ice-loss processes ( Conway et al., 2019a).įigure 9.14. Channels incising into and emanating from ejecta blankets are used as evidence for water escaping from the melting cryosphere beneath ( Fig. 9.14C and D) ( El-Maarry et al., 2013 Harrison et al., 2010 Jones et al., 2011 Mangold, 2012 Weiss et al., 2017). These pits can be associated with incised channels, alluvial fans ( Fig. 9.14F), and debris lobes emanating from high points inside the crater cavity, thought to represent the flow of water-rich materials immediately post-impact, for example, alluvial fans in Tooting and Mojave Craters both dated to <10 Ma ( Goddard et al., 2014 Morris et al., 2010 Williams and Malin, 2008). Craters only a few million years old display pits on their floors ( Fig. 9.14A) and within their ejecta materials interpreted to be a result of volatile-release as steam ( Boyce et al., 2012 Morris et al., 2010 Mouginis-Mark and Boyce, 2012 Tornabene et al., 2012). Geomorphological evidence for these processes in the Amazonian epoch is abundant. This could be melting immediately during the impact in the cavity and the ejecta ( Boyce et al., 2012 Newsom, 1980 Weiss and Head, 2016), vaporization of the ice could inject vapor into the surrounding atmosphere and create a transient and localized hydrological cycle ( Kite et al., 2011 Segura, 2002 Segura et al., 2008 Steakley et al., 2019), and finally the thermal anomaly could maintain hydrothermal circulation within the crust for thousand or millions of years postimpact ( Abramov and Kring, 2005 Barnhart et al., 2010 Osinski et al., 2013 Rathbun and Squyres, 2002). As discussed in Section 2, we know that there are substantial amounts of water ice in the near-surface of the Martian crust and potentially a deep cryosphere, and so the heat deposited into the crust by impacts could generate liquid water by melting. The lack of substantial atmosphere on Mars means that bolides reach the surface with greater energy than they do on Earth. Hypervelocity impacts by bolides into planetary surfaces deposit huge amounts of energy into the target body, of which most is converted into heat ( Melosh, 1989). Stillman, in Mars Geological Enigmas, 2021 3.7 Liquid water–related morphologies associated with impact craters