Topographic Analysis of the Asymmetric Ejecta of Zunil Crater, Mars
Abstract
The 10.1 km diameter crater Zunil (7.7oN, 166.2oE) has many of the attributes of a fresh impact crater on Mars, including pitted material on the crater floor, an extensive field of secondary craters, as well as thermally-distinct crater rays. But unlike most craters of this size and location, Zunil crater displays a striking azimuthal variation in ejecta deposits with both fluidized and ballistic ejecta. Here we investigate the geometric attributes of the crater cavity and rim to try to identify the cause of this ejecta asymmetry, as well as the possible explanation for the formation of the ballistic ejecta. To accomplish this, we have created a digital elevation model (DEM) from stereo Context Camera (CTX) images, using the Ames Stereo Pipeline software. We used CTX frames F06_038250_1877 and G05_020211_1877 to produce a DEM with a nominal spatial resolution of 24 m/pixel, and use this DEM to conduct a detailed morphometric analysis of the crater in order to ascertain the nature of this "lobate-ballistic ejecta dichotomy", as well as derive new information on local target properties and the nature of the impact process itself. Measuring the rim height and radius at one-degree increments of azimuth, we find there are numerous places on the rim crest that are both higher and wider, or lower and narrower, than is typical for Zunil crater. There are places where rim height and radius are both close to average, while in other places both the rim height and radius are larger or smaller than the average. There is also a lack of consistency between the geometry of the crater and the type of ejecta; namely no direct correlation between rim height, crater radius, and ejecta type, but a slight negative correlation between radius and rim height for parts of the crater which possess ballistic ejecta. We find good circumstantial evidence that some of the target rock within which Zunil crater formed may have been dry at the time of impact compared to other craters of this size, latitude and elevation. We speculate that this lack of volatiles most likely arose from the drainage of water to depths greater than the excavation depth of Zunil crater. The asymmetric nature of the ejecta blanket argues strongly against the notion that the Martian atmosphere was partially responsible for ejecta fluidization.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2016
- Bibcode:
- 2016AGUFM.P11E..01M
- Keywords:
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- 6299 General or miscellaneous;
- PLANETARY SCIENCES: SOLAR SYSTEM OBJECTSDE: 5464 Remote sensing;
- PLANETARY SCIENCES: SOLID SURFACE PLANETSDE: 5470 Surface materials and properties;
- PLANETARY SCIENCES: SOLID SURFACE PLANETSDE: 5499 General or miscellaneous;
- PLANETARY SCIENCES: SOLID SURFACE PLANETS