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. 2017 Jul 15;44(13):6570–6578. doi: 10.1002/2017GL073970

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©2017. The Authors.

This is an open access article under the terms of the Creative Commons Attribution‐NonCommercial‐NoDerivs License, which permits use and distribution in any medium, provided the original work is properly cited, the use is non‐commercial and no modifications or adaptations are made.

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Comparison of pitted terrains on Mars, Vesta, and Ceres. (a) Pitted terrain within the 10.3 km diameter Zunil Crater (7.70°N/166.19°E) on Mars as seen in HiRISE image ESP_038250_1880 (0.25 m/pixel). (b) Pitted terrain within the 67.6 km diameter Marcia Crater (8.98°N/339.55°E) on Vesta as seen in Framing Camera images 14,662 (19.7 m/pixel). Pitted terrains observed on Ceres are highlighted in (c) Haulani Crater, (d) Ikapati Crater, and (e) Dantu Crater; Framing Camera nadir mosaic (30 m/pixel). (e) Lines indicating the shared borders of the Dantu pits; see Figure 3 of Boyce et al. [2012] for comparison. Scale bar indicates 1 km in all images. Note that north is not up.