Other
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p13d1732h&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P13D-1732
Other
[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [5422] Planetary Sciences: Solid Surface Planets / Ices, [5494] Planetary Sciences: Solid Surface Planets / Instruments And Techniques, [6250] Planetary Sciences: Solar System Objects / Moon
Scientific paper
Neutron spectroscopy from Lunar Prospector returned data consistent with the presence of water ice in the near-subsurface of the Moon in permanently shadowed regions (PSRs) at low spatial resolution. Clementine and ground-based radar returned tantalizing, but inconclusive evidence of ice in lunar PSRs. Later, Mini-RF on Chandrayaan-1 and LRO detected a signature consistent with water ice in some polar craters on the Moon, but not all PSRs. Similarly, LEND on LRO detected a heterogeneous distribution of hydrogen among lunar PSRs. In addition, LAMP on LRO detected FUV spectra consistent with a heterogeneous distribution of frost on the surface of permanently shadowed regions. Yet the weakest spectral feature from LAMP was associated with the crater with the strongest hydrogen feature from LEND. The impact of LCROSS into Cabeus released water and other volatiles, but abundances were higher than the background amounts detected by neutron spectroscopy implying heterogeneity within that PSR. Data from any one instrument taken alone would lead one to a different conclusion about the distribution of volatiles than data taken from any other single instrument. Although the data from different instrumentation can seem to be disparate, the apparent discrepancy results from the different fields of view and sensitivities of the detection techniques. The complementary nature of these data can be exploited to provide a multi-dimensional view of volatiles in lunar PSRs. We apply a Monte Carlo model to describe the retention and redistribution of volatiles within lunar cold traps. The model runs constrain the coherence of volatile deposits with depth, area, and time, which allows us to examine how a given volatile distribution would appear to remote sensing experiments. This provides a big picture framework for integrating the observations of volatiles on the surface and at depth at the poles of the Moon with the goal of finding a distribution of volatiles in lunar PSRs consistent with all of the data.
Bussey Ben
Elphic Richard C.
Gladstone Randy
Hurley Dana M.
Lawrence D. Jr. J.
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