Planetary Surface Processes

By Philip A. Bland, S. Schwenzer. 2018

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Geologic Constraints on Early Mars Climate (2018, background): “2016), but rounded hill-crests can form due to non-rainfall processes (Melosh 2009).”
Enceladus's and Dione's floating ice shells supported by minimum stress isostasy (2016, background): “The average crustal stress is about 30 kPa for Enceladus, which is half of the average topographic stress, as expected in isostasy [Melosh, 2011].”
Generation, ascent and eruption of magma on the Moon:new insights into source depths, magma supply, intrusions and effusive/explosive eruptions (Part 2: Predicted Emplacement Processes and Observations) (2017, background): “chains formed from projectile disruption during close approach to Earth are unlikely to occur on the lunar farside (Melosh and Whitaker, 1994). Although Wilhelms and Hodges (1978) pointed out that the Mendeleev crater chain is radial to Tsiolkovsky crater, ~850 km away, no other similar examples rad”