Ridge-like lava tube systems in southeast Tharsis, Mars

Geological Characteristics and Targets of High Scientific Interest in the Zhurong Landing Region on Mars

“…Various formation mechanisms have been proposed for linear or curvilinear ridges on the martian surface, including inverted fluvial channels (e.g., Burr et al., 2009; Williams et al., 2013), linear dunes (e.g., Davis et al., 2020; Ruff, 1994), lava tubes (e.g., Zhao et al., 2017), igneous dikes (e.g., Huang et al., 2012; Korteniemi et al., 2010), eskers (e.g., Banks et al., 2009; Kress & Head, 2015), or etc. The ridges in the study region are composed of rocky materials and have variable orientations, which is not consistent with a linear dune origin.…”

“…Could the ridges be formed by igneous processes (e.g., Head et al, 2006)? The Type 1 ridges are usually short and straight, and similar features have been interpreted as igneous dikes (Korteniemi et al, 2010); Type 2 ridges are longer and more sinuous, which may be similar with the ridge-like lava tubes identified in the Tharsis region (Zhao et al, 2017). In addition, an esker origin for Type 2 ridges could not be easily eliminated considering their sinuous form and the ability to cross topographic divides (Banks et al, 2009).…”

Inverted channel belts and floodplain clays to the East of Tempe Terra, Mars: Implications for persistent fluvial activity on early Mars

“…Several interpretations have been proposed for sinuous ridges on Mars, including lava tubes, eskers, inverted channels, and inverted channel belt [Bernhardt et al, 2013;Bernhardt et al, 2019;Bleacher et al, 2017;Davis et al, 2019;Gallagher and Balme, 2015;Guidat et al, 2015;Hayden et al, 2019;Lefort et al, 2012;Newsom et al, 2010;Pain et al, 2007;Ramsdale et al, 2015;Williams et al, 2013;Zealey, 2009;Zhao et al, 2017]. Lava tubes are mostly associated with volcanic activities and lava flows.…”

Distribution and Morphology of Lava Tube Systems on the Western Flank of Alba Mons, Mars

“…Surface features include elongate collapse depressions and local sources (lava ponds or small vents for breakout flows). The close association of lava tubes and flow inflation processes (e.g., Self et al., 1998). High‐resolution images now reveal characteristics of Martian lava flows with flow morphologies indicative of inflation and pahoehoe‐like, compound emplacement scenarios (Bleacher et al., 2017; Crown & Ramsey, 2017; Giacomini et al., 2009; Hamilton et al., 2018, 2020; Keszthelyi et al., 2000, 2006; Zhao et al., 2017). Inflated flows can be used to search for and identify potential upslope lava tubes related to their emplacement.…”