Mathematics – Logic
Scientific paper
May 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agusm.p13a..05s&link_type=abstract
American Geophysical Union, Spring Meeting 2009, abstract #P13A-05
Mathematics
Logic
1221 Lunar And Planetary Geodesy And Gravity (5417, 5450, 5714, 5744, 6019, 6250), 5420 Impact Phenomena, Cratering (6022, 8136), 5462 Polar Regions, 5464 Remote Sensing, 5480 Volcanism (6063, 8148, 8450)
Scientific paper
The Schrödinger impact basin is located on the lunar far side near the south pole (76oS, 134oE) and is one of only two young multiring impact basins on the lunar surface [1]. With a diameter size of 312 km and basin floor 2-3 km deep, Schrödinger is the least modified impact basin of its size. A peak ring structure 150 km in diameter lies on the basin floor, formed by uplift of pre-Schrödinger crustal materials. Ejecta material, smooth in texture, covers the basin walls and extends out onto the surrounding surface up to 100 km in all directions. The first geological map published of Schrödinger was generated using preliminary Clementine data [1]. The map described the geology and geomorphology within the inner basin with smooth and rough plains of shocked material occupying most of the basin floor. The rough plains are identified by presence of hummocks, swales, and low knobs. Smooth plains have no discernable features identifiable. Ghost craters are found along both smooth and rough patches. A volcanic vent in the inner eastern corner of Schrödinger is interpreted as a source for pyroclastic eruptions within the area. Located along the volcanic vent is a north-east trending graben. There are thin patches of impact melt sheets along the basin walls and peak ring. A lobate ridge located near the centre of the inner basin is interpreted as having formed by buckling of the melt sheet. A more recent geologic map using high resolution Clementine UVVIS data and topography data is in agreement with the proposed geology within the Schrödinger basin [2]. Contacts between various units are better outlined in the recent map. Using spectra derived from high resolution Clementine UVVIS images and Lunar Prospector data we determine the composition of impact melt, impact ejecta, and the extent of proposed cryptomare deposits [3]. We also use Fe, Th, and Ti abundance in determining the composition of these units. Our goal is to determine the abundance and distribution of impact melt relative to volcanic products and ejecta units. We are also addressing possible differentiation of the melt sheet as a crater the size of Schrödinger has sufficient time to cool and allow for melt to differentiate. References: [1] Shoemaker, E.M., Robinson, M.S., and Eliason, E.M. (1994) Science. 266. 1851- 1854. [2] Mest, S. C.; Van Arsdall, L. E. (2008) NLSI Lunar Science Conference. Abstract 2089. [3] Antonenko, I. (1999) PhD Thesis, Brown University. Chapter 4, pp 13-14.
Antonenko Irene
Osinski Gordon
Shankar B.
Stooke Philip J.
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