The rim or edge of an impact crater is the part that extends above the height of the local surface, usually in a circular or elliptical pattern. In a more specific sense, the rim may refer to the circular or elliptical edge that represents the uppermost tip of this raised portion. If there is no raised portion, the rim simply refers to the inside edge of the curve where the flat surface meets the curve of the crater bottom.
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Simple craters
Smaller, simple craters retain rim geometries similar to the features of many craters found on the Moon and the planet Mercury.[1]
Complex craters
Large craters are those with a diameter greater than 2.3 km, and are distinguished by central uplifts within the impact zone.[1] These larger (also called “complex”) craters can form rims up to several hundred meters in height.
A process to consider when determining the exact height of a crater rim is that melt may have been pushed over the crest of the initial rim from the initial impact, thereby increasing its overall height. When combined with potential weathering due to atmospheric erosion over time, determining the average height of a crater rim can be somewhat difficult.[2] It has also been observed that the slope along the excavated interior of many craters can facilitate a spur-and-gully morphology, including mass wasting events occurring due to slope instability and nearby seismic activity.[3]
Complex crater rims observed on Earth have anywhere between 5X – 8X greater height:diameter ratio compared to those observed on the Moon, which can likely be attributed to the greater force of gravitational acceleration between the two planetary bodies that collide.[1] Additionally, crater depth and the volume of melt produced in the impact are directly related to the gravitational acceleration between the two bodies.[4] It has been proposed that “reverse faulting and thrusting at the final crater rim [is] one of the main contributing factors [to] forming the elevated crater rim”.[2] When an impact crater is formed on a sloped surface, the rim will form in an asymmetric profile.[5] As the impacted surface's angle of repose increases, the crater's profile becomes more elongate.
Classification
The rim type classifications are full-rim craters, broken-rim craters, and depressions.[5]
References
- ^ a b c Pike, R.J. (1981). "Meteorite Craters: Rim Height, Circularity, and Gravity Anomalies". Lunar and Planetary Science. XII: 842–844. Bibcode:1981LPI....12..842P.
- ^ a b Krüger, T., Kenkmann, T., & Hergarten, S. (2017). "Structural Uplift and Ejecta Thickness of Lunar Mare Craters: New Insights Into the Formation of Complex Crater Rims". Meteoritics & Planetary Science. 52 (10): 2220–2240. Bibcode:2017M&PS...52.2220K. doi:10.1111/maps.12925. S2CID 135227558.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ Krohn, K., Jaumann, R., Otto, K., Hoogenboom, T., Wagner, R., Buczkowski, D., Schenk, P. (2014). "Mass Movement on Vesta at Steep Scarps and Crater Rims". Icarus. 244: 120–132. Bibcode:2014Icar..244..120K. doi:10.1016/j.icarus.2014.03.013. hdl:2286/R.I.28057. S2CID 2313339.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ Neish, C., Herrick, R., Zanetti, M., & Smith, D. (2017). "The Role of Pre-Impact Topography in Impact Melt Emplacement on Terrestrial Planets". Icarus. 297: 240–251. Bibcode:2017Icar..297..240N. doi:10.1016/j.icarus.2017.07.004.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ a b Hayashi, K.; Sumita, I. (2017). "Low-Velocity Impact Cratering Experiments in Granular Slopes". Icarus. 291: 160–175. Bibcode:2017Icar..291..160H. doi:10.1016/j.icarus.2017.03.027.
This page was last edited on 29 September 2023, at 14:35