Figure - PMC

Skip to main content

An official website of the United States government

Here's how you know

Here's how you know

Official websites use .gov
A .gov website belongs to an official government organization in the United States.

Secure .gov websites use HTTPS
A lock ( ) or https:// means you've safely connected to the .gov website. Share sensitive information only on official, secure websites.

View full-text article in PMC

. 2020 Sep 15;20(9):1121–1149. doi: 10.1089/ast.2019.2203

Search in PMC
Search in PubMed
View in NLM Catalog
Add to search

© G.R. Osinski et al., 2020; Published by Mary Ann Liebert, Inc.

This Open Access article is distributed under the terms of the Creative Commons License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly credited.

PMC Copyright notice

FIG. 1. — Images of impact craters showing the change in morphology with increasing size. (A) The 3 km diameter Zumba Crater on Mars, a prototypical simple crater. Note the impact ejecta deposits (“e”) and the impact melt deposits (“m”) on the crater floor. Portion of Mars Reconnaissance Orbiter High Resolution Imaging Science Experiment (HiRISE) image PSP_003608_1510. NASA/JPL/University of Arizona. (B) The 93 km diameter Pettit Crater on Mars, a well-preserved complex crater with a central peak (“cp”). THEMIS day-time mosaic. NASA/JPL/Arizona State University. (C) With increasing diameter, central peaks are replaced by peak-rings (“pr”) as in the case of the ∼320 km diameter Schrödinger Crater on the Moon. The crater has well-preserved ejecta deposits, and impact melt occurs both inside and outside the peak-ring. Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) mosaic. NASA/JPL/ASU. (D) The largest impact features in the Solar System are termed impact basins, such as the ∼900 km diameter Orientale Basin on the Moon shown here. It contains three ring features labeled 1–3. LRO WAC mosaic. NASA/JPL/ASU.