Surface refreshing of Martian moon Phobos by orbital eccentricity-driven grain motion View Full Text


Ontology type: schema:ScholarlyArticle     


Article Info

DATE

2019-04

AUTHORS

Ronald-Louis Ballouz, Nicola Baresi, Sarah T. Crites, Yasuhiro Kawakatsu, Masaki Fujimoto

ABSTRACT

The surface of the Martian moon Phobos exhibits two distinct geologic units, red and blue, characterized by their spectral slopes. The provenance of these units is uncertain yet crucial to understanding the origin of the Martian moon and its interaction with the space environment. Here we present a combination of dynamical analyses and numerical simulations of particle dynamics to show that periodic variations in dynamic slopes, driven by orbital eccentricity, can cause surface grain motion. For regions with steep slopes that vary substantially over one Phobos orbit, the surface is excavated at a faster rate than the space weathering timescale. Our model predicts that this new mechanism is most effective in regions that coincide with blue units. Therefore, space weathering is the likely driver of the dichotomy on the moon’s surface, reddening blue units that represent pristine endogenic material. The distribution of two distinct geologic units on Mars’s moon Phobos – red and blue units – can be explained by surface grain motion triggered by orbital variations in slope steepness, according to dynamical analyses and numerical simulations. More... »

PAGES

229-234

References to SciGraph publications

Identifiers

URI

http://scigraph.springernature.com/pub.10.1038/s41561-019-0323-9

DOI

http://dx.doi.org/10.1038/s41561-019-0323-9

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54 schema:description The surface of the Martian moon Phobos exhibits two distinct geologic units, red and blue, characterized by their spectral slopes. The provenance of these units is uncertain yet crucial to understanding the origin of the Martian moon and its interaction with the space environment. Here we present a combination of dynamical analyses and numerical simulations of particle dynamics to show that periodic variations in dynamic slopes, driven by orbital eccentricity, can cause surface grain motion. For regions with steep slopes that vary substantially over one Phobos orbit, the surface is excavated at a faster rate than the space weathering timescale. Our model predicts that this new mechanism is most effective in regions that coincide with blue units. Therefore, space weathering is the likely driver of the dichotomy on the moon’s surface, reddening blue units that represent pristine endogenic material. The distribution of two distinct geologic units on Mars’s moon Phobos – red and blue units – can be explained by surface grain motion triggered by orbital variations in slope steepness, according to dynamical analyses and numerical simulations.
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