Miranda's Thick Regolith Indicates a Major Mantling Event from an Unknown Source - IOPscience

1. Background1.1. Miranda's GeologyThe Uranian satellite Miranda has a complex surface, with multiple large regions of intense deformation called"coronae" that were likely formed by tectonism and might be at least partially cryovolcanic in origin as well . Miranda also displays a Global Rift System, composed of large sets of faults and fractures, that cut across its surface and bound the coronae .

1.2. Impact Crater Modification across the Solar SystemThe morphologies of impact craters can be altered by one or more types of processes that are identifiable in remotely sensed imaging data sets.

1.2.2. Degraded CratersWhere erosional processes are dominant, mass-wasting and/or aeolian activity continuously expose the crater rims, revealing the bedrock/bed-ice and ). During degradation, erosional processes are able to efficiently break apart high-standing craters rims, depositing much of this rim material downslope on the low-lying crater floor, thereby keeping the rim mostly exposed while burying the crater interior .

2. Miranda's Muted Craters and Scarps2.1. Identification and Comparison of Muted and Non-muted FeaturesMiranda's cratered terrains show examples of both non-muted and muted craters and scarps . As summarized in Table 1, non-muted craters have relatively sharp and prominent rims, whereas muted craters have rounded and more subtle rims .

In some locations, non-muted tectonic features exhibit trends consistent with trends of muted tectonic features . For example, alternating sections of muted and non-muted scarps make up the 340° Chasma. Relatively non-muted tectonic features also exhibit orientations concentric and radial to Arden Corona and ).

3. Estimating Miranda's Regolith Thickness3.1. Crater d-D RatiosWe investigated examples of non-muted and muted craters within Miranda's cratered terrain region immediately north of Inverness Corona and the SPT Chasma. This area was imaged at relatively high resolution in comparison with other cratered terrain regions on Miranda, allowing us to derive a more precise and higher-resolution digital elevation model compared to other regions .

As derived from physical laboratory experiments , and utilized to estimate lunar regolith thicknesses , the thickness of a pre-existing layer of regolith that experiences an impact event can be estimated using central mounds on their floors . In a non-muted crater with a central mound, tr is estimated by

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