Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p53c1529b&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P53C-1529
Mathematics
Logic
[5470] Planetary Sciences: Solid Surface Planets / Surface Materials And Properties, [5475] Planetary Sciences: Solid Surface Planets / Tectonics, [6063] Planetary Sciences: Comets And Small Bodies / Volcanism, [6235] Planetary Sciences: Solar System Objects / Mercury
Scientific paper
The Caloris basin on Mercury is floored by light-toned plains and surrounded by an annulus of dark-toned material interpreted to be ejecta blocks and smooth, dark, ridged plains. Strangely, preliminary crater-counts indicate that these intra-ejecta dark plains are younger than the light-toned plains within the Caloris basin. This would imply a second, younger plains emplacement event, possibly involving lower albedo material volcanics, which resurfaced the original ejecta deposit. On the other hand, the dark plains may be pre-Caloris light plains covered by a thin layer of dark ejecta. Another alternative to the hypothesis of young, dark volcanism is the possibility that previous crater-counts have not thoroughly distinguished between superposed craters (fresh) and partly-buried craters (old) and therefore have not accurately determined the ages of the Caloris units. We here outline the tasks associated with a new mapping project of the Caloris basin, intended to improve our knowledge of the geology and geologic history of the basin, and thus facilitate an understanding of the thermal evolution of this region of Mercury. We will 1) classify craters based on geomorphology and infilling, 2) create a high-resolution map of the intra-ejecta dark plains, 3) perform crater counts of the intra-ejecta dark plains, the ejecta, and the Caloris floor light plains and 4) refine the stratigraphy of Caloris basin units. We will use new high resolution (200-300 m/p) imaging data from the MDIS instrument to create a new geomorphic map of the dark annulus around the Caloris basin. Known Caloris group formations will be mapped where identified and any new units will be defined and mapped as necessary. Specifically, we will delineate hummocks and smooth plains within the Odin formation and map them separately. We will look for unequivocal evidence of volcanic activity within the dark annulus and the Odin Formation, such as vents and flow lobes. The location of any filled craters will be especially noted, to be incorporated into a new crater classification scheme that includes both degradation state and level and type of infilling. We will also distinguish between craters infilled with 1) lava, 2) impact melt and 3) ejecta, based on our interpretation of the MDIS images. We will then determine the crater size-frequency distribution of each geomorphic unit. We will analyze the crater density of the Caloris floor plains unit, the Odin Formation ejecta and the Odin Formation intra-ejecta dark plains. We will do a second count of Caloris floor craters that includes filled craters, to attempt to get a minimum age for the underlying dark basement. Crater counting on any additional geologic units will depend upon results of the geomorphic mapping. Finally, we will refine the stratigraphy of the Caloris basin units. We start in the region where MESSENGER data over-laps Mariner 10 images. By comparing the Caloris group formations mapped in the Tolstoj and Shakespeare quadrangles to the overlapping MDIS images, we determine the distinctive geomorphology of each of these units in the high resolution MESSENGER data. We will then use this as diagnostic criteria as we map the rest of the basin.
Buczkowski D.
Seelos Kim D.
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