Source: Journal of Geophysical Research: Planets
Water ice on Mars is not currently stable in the near-equatorial regions of the planet, yet features hypothesized to require the presence of volatiles in the subsurface to form have been well-known for decades. Layered-ejecta craters (once termed ‘fluidized-ejecta craters’ and ‘rampart craters’) have distinct patterns of their ejecta produced during the impact event. These ejecta shapes appear to result from an impact into materials mixed with subsurface ice. Kirchoff and Grimm  investigate a subset of these craters and find that layered-ejecta craters near the equator of Mars have formed in each of the planet’s major time epochs, implying ice has even been present geologically recently. However, the authors also find that these layered-ejecta craters are interspersed with craters with more typical ejecta patterns not associated with subsurface ice indicating that the preservation of such ice has been heterogeneous in both location and time. Understanding the distribution and ages of these craters is an important step towards unraveling past climate on Mars and the ability of the surface to preserve that history through time.
Citation: Kirchoff, M. R., & Grimm, R. E. . Timing and distribution of single-layered ejecta craters imply sporadic preservation of tropical subsurface ice on Mars. Journal of Geophysical Research: Planets, 123. https://doi.org/10.1002/2017JE005432
—Steven A. Hauck II, Editor-in-Chief, JGR: Planets
Correction, 15 February 2018: An earlier version of this article included an additional author name in the image credit. This has been removed.
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