Dynamic cooling experiments on a synthetic martian lava reveal a history quite similar to that of pāhoehoe flows on Earth.
Experimenting with the 1-atm gas-mixing furnace in the experimental petrology lab of the University of Hawaii, I re-created different cooling scenarios for this martian lava, which is based on the bulk composition of meteorite Yamato 980459. At least two stages of cooling were necessary to reproduce the textures and compositions of phases in the meteorite.
It is likely that pyroxene and olivine phenocrysts began crystallizing at depth and grew further upon eruption, at ~10 °C h-1 . Subsequent crystallization of groundmass pyroxene and olivine would have occurred at cooling rates of ~100 °C h-1. These cooling rates are consistent with different depths in a pāhoehoe-like lava flow. High resolution remote sensing imagery from Mars strongly suggests the presence of large, sheet-like flows with inflated margins, making this conclusion plausible.
Publication: First, E., Hammer, J. (2016) Igneous cooling history of olivine-phyric shergottite Yamato 980459 constrained by dynamic crystallization experiments. Meteoritics and Planetary Science,51, 1233-1255.