Imperial College London
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Professor Gareth Collins

Faculty of Engineering, Department of Earth Science & Engineering

Professor of Planetary Science
 
 
 
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Contact

 

+44 (0)20 7594 1518g.collins Website

 
 
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Location

 

4.83Royal School of MinesSouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@article{Daubar:2022:10.1029/2021je007145,
author = {Daubar, IJ and Dundas, CM and McEwen, AS and Gao, A and Wexler, D and Piqueux, S and Collins, GS and Miljkovic, K and Neidhart, T and Eschenfelder, J and Bart, GD and Wagstaff, K and Doran, G and Posiolova, L and Malin, M and Speth, G and Susko, D and Werynski, A},
doi = {10.1029/2021je007145},
journal = {Journal of Geophysical Research: Planets},
pages = {1--21},
title = {New craters on Mars: an updated catalog},
url = {http://dx.doi.org/10.1029/2021je007145},
volume = {127},
year = {2022}
}
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RIS format (EndNote, RefMan)

TY  - JOUR
AB  - We present a catalog of new impacts on Mars. These craters formed in the last few decades, constrained with repeat orbital imaging. Crater diameters range from 58 m down to <1 m. For each impact, we report whether it formed a single crater or a cluster (58% clusters); albedo features of the blast zone (88% halos; 64% linear rays; 10% arcuate rays; majority dark-toned; 4% light-toned; 14% dual-toned); and exposures of ice (4% definite; 2% possible). We find no trends in the occurrences of clusters with latitude, elevation, or impact size. Albedo features do not depend on atmospheric fragmentation. Halos are more prevalent at lower elevations, indicating an atmospheric pressure dependence; and around smaller impacts, which could be an observational bias. Linear rays are more likely to form from larger impacts into more consolidated material and may be enhanced by lower atmospheric pressure at higher elevations. Light- and dual-toned blast zones occur in specific regions and more commonly around larger impacts, indicating excavation of compositionally distinct material. Surfaces covered with bright dust lacking cohesion are favored to form detectable surface features. The slope of the cumulative size frequency distribution for this dataset is 2.2 for diameters >8 m (differential slope 2.9), significantly shallower than the slope of new lunar craters. We believe that no systematic biases exist in the martian dataset sufficient to explain the discrepancy. This catalog is complete at the time of writing, although observational biases exist, and new discoveries continue.
AU  - Daubar,IJ
AU  - Dundas,CM
AU  - McEwen,AS
AU  - Gao,A
AU  - Wexler,D
AU  - Piqueux,S
AU  - Collins,GS
AU  - Miljkovic,K
AU  - Neidhart,T
AU  - Eschenfelder,J
AU  - Bart,GD
AU  - Wagstaff,K
AU  - Doran,G
AU  - Posiolova,L
AU  - Malin,M
AU  - Speth,G
AU  - Susko,D
AU  - Werynski,A
DO  - 10.1029/2021je007145
EP  - 21
PY  - 2022///
SN  - 2169-9097
SP  - 1
TI  - New craters on Mars: an updated catalog
T2  - Journal of Geophysical Research: Planets
UR  - http://dx.doi.org/10.1029/2021je007145
UR  - https://agupubs.onlinelibrary.wiley.com/doi/10.1029/2021JE007145
UR  - http://hdl.handle.net/10044/1/98223
VL  - 127
ER  -
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