Small‐scale Martian polygonal terrain: Implications for liquid surface water

By N. Seibert, J. Kargel. 2001

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The rayed crater Zunil and interpretations of small impact craters on Mars (2005, background): “, 2004) , polygonal terrain(Siebert and Kargel, 2001) , glaciers(Kargel, 2004; Neukum et al 2004), lava flows and rootless cones (Keszthelyi et al.”
Icelandic analogs to Martian flood lavas (2004, background): “It is noteworthy that these polygons are quite morphologically distinct from polygons found elsewhere on Mars that are interpreted to be caused by ice and/or water [e.g., Rossbacher and Judson, 1981; Seibert and Kargel, 2001].”
High latitude patterned grounds on Mars: Classification, distribution and climatic control (2005, background): “these two groups, except large polygons geographically restricted to Elysium and Utopia (Seibert and Kargel, 2001).”
Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations (2009, background): “Fractures may arise from several processes hypothesized to be active on Mars, including (1) thermal contraction of ice/ice-cemented sediments [Lachenbruch, 1962; Lucchitta, 1981; Mellon, 1997; Seibert and Kargel, 2001; Mangold, 2005; Levy et al., 2008b]; (2) thermal contraction of lava/magma [Mutch ”