Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p33g..03f&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P33G-03
Mathematics
Logic
[5420] Planetary Sciences: Solid Surface Planets / Impact Phenomena, Cratering, [5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6235] Planetary Sciences: Solar System Objects / Mercury, [6250] Planetary Sciences: Solar System Objects / Moon
Scientific paper
The formation of large impact basins played a critical role in the early evolution of the surfaces of Mercury and the Moon. New data from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) and Lunar Reconnaissance Orbiter (LRO) missions have enabled a re-evaluation of the sequence and chronology of large impact basin formation and modification on both planets, as well as global characterization of the crater density on the surface of each planetary body for craters of diameter D ≥ 20 km. These observations allow us to understand how basins are superposed by volcanic plains on each planet, and the similarities and differences in volcanic resurfacing that these crater densities imply. From this record, it appears that even the most densely cratered regions on Mercury have fewer craters per unit area between 20 km and ~100 km in diameter than the Moon, a difference that reflects widespread volcanic resurfacing on Mercury early in its history. For craters and basins with D ≥ 100 km, the density of superposed craters on Mercury in a given size range is similar to that of the Moon. Because such large craters are less easily removed by volcanic resurfacing, we interpret this similarity to be the result of impact saturation effects on both bodies. However, on Mercury, it appears that all large basins (D > 500 km) experienced substantial volcanic modification after their formation, in contrast with the Moon, where some basins remain relatively unfilled. Further observations of the interactions of basins and volcanism on each body will enable a deeper understanding of their planetary-scale geophysical and geological evolution.
Dickson James L.
Fassett Caleb I.
Head James W.
Hurwitz Debra M.
Kadish Seth J.
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