Figure 23. FRT00021C92-based false color image with 50% transparency over red version of the HiRISE mosaic. The figure covers the SoF and eastern side of the Greenheugh pediment. Arrow represents inferred wind direction for sands derived from SoF and deposited on the pediment, together with local bedrock-derived sediment also blown onto the pediment. RGB set to 0.618, 0.553, 0.468 µm. Slopes >15° were excised from the FRT image to enhance the color variations associated with relatively flat terrain.
Second, there is a potential that these two deposits have different source materials. In our study, olivine is the heaviest mineral with augite and pigeonite having approximately equal densities. Topographic influence and wind sorting alone may not be enough to explain the variation in pyroxene abundances observed through spectral modeling results, as wind sorting would not separate the pyroxene minerals. The combination of unique source material and topographic influence, however, could then explain the outcomes of this study observed from spectral data. In this case, SoF would have been sourced from a more augite-rich material compared to MDI.
Finally, our result has implications for interpreting aeolian deposits in the Martian rock records. Here we have two sand bodies that are close to one another yet have different properties. This is an example of the paradigm that “present is the key to the past”. The aeolian rock record likely has similar examples of deposits in the same stratigraphic horizon, but with laterally varying properties controlled by local topographic or other controls. Unique properties observed within aeolian rocks could provide insights into more regional variations of topography, wind regime, and mineral sorting.
9 Acknowledgments
The work presented in this paper was partially supported by Contract 1549716 from the Caltech/Jet Propulsion Laboratory to REA, MNH, and SJV, for participation on the Mars Science Laboratory Curiosity rover mission. RVM acknowledges support from the NASA Mars Science LaboratoryCuriosity rover mission and the NASA Johnson Space Center. We thank Loan Le (Jacobs, Johnson Space Center) for synthesis and electron microprobe analyses of synthetic glasses.
10 Data Availability Statement
The data sets used in this study are publicly available through the Planetary Data System Geosciences Node (https://pds-geosciences.wustl.edu/). The HiRISE data are available at https://www.uahirise.org/. CRISM, Navcam, Mastcam, MARDI, MAHLI, and APXS raw data can be found at https://pds-geosciences.wustl.edu/dataserv/doi.htm. Mastcam, MAHLI, and MARDI mosaics were processed by the Mastcam team at Malin Space Science Systems (MSSS). Laboratory mineral spectra are available through the PDS/RELAB (https://pds-speclib.rsl.wustl.edu/) and the USGS (https://www.usgs.gov/labs/spectroscopy-lab/science/spectral-library) spectral libraries, while the synthetic glass spectra can be found at https://openscholarship.wustl.edu/data/102/. The product IDs and DOIs of all data sets used in this study are also listed in Table 1.
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