Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p41a1591h&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P41A-1591
Mathematics
Logic
[5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6235] Planetary Sciences: Solar System Objects / Mercury
Scientific paper
Volcanism has been conclusively identified on the surface of Mercury from images and color data collected by the Mercury Dual Imaging System (MDIS) instrument aboard the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft. Most of the volcanic deposits on Mercury are similar in morphology to lunar mare flood basalt deposits and are found on Mercury in smooth plains regions such as in the extensive northern smooth plains. Adjacent to the northern smooth plains is an unusual assemblage of 5-10-km-diameter pits, teardrop-shaped hills, rough plains, and distal lobate-margined smooth plains; these features are interpreted to represent source vents, lava sculpting of underlying terrain, and distal emplacement of extensive flow lobes. These features are consistent with eruption of high-temperature, low-viscosity komatiite-like flood lavas that erode and sculpt the underlying terrain during flow on Mercury. Evidence of this process is observed extensively on other terrestrial planets where eroded channels are often seen in association with source depressions. Here we analyze Mercury Laser Altimeter (MLA) data and MDIS images to document morphologic and morphometric constraints on the amount of erosion that occurred and the amount of lava that was emplaced during the formation of this scoured surface. These constraints are used as inputs into models of mechanical and thermal erosion to determine which erosion regime, mechanical or thermal, was dominant during the formation of this terrain, as well as to determine plausible erosion rates and eruption durations required to form the observed scoured terrain. We compare processes of volcanism and thermal/mechanical erosion on Mercury with similar processes on Earth, the Moon, Mars and Venus.
Baker Mark D.
Blewett Dave T.
Byrne Paul K.
Chabot Nancy Lynne
Denevi Brett Wilcox
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