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| Titel |
Estimated Rock Abundances at the Apollo and Luna Landing Sites |
| VerfasserIn |
Karin E. Bauch, Harald Hiesinger, Julia Weinauer, Mark S. Robinson, Frank Scholten |
| Konferenz |
EGU General Assembly 2013
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| Medientyp |
Artikel
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| Sprache |
Englisch
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| Digitales Dokument |
PDF |
| Erschienen |
In: GRA - Volume 15 (2013) |
| Datensatznummer |
250079204
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| Zusammenfassung |
| Diurnal temperature variations can be used to analyze the surface and subsurface
thermophysical properties [1, 2]. These properties, namely the bulk density, heat capacity,
and thermal conductivity, define the thermal inertia, which represents the ability
of the surface and subsurface to conduct and store heat [2]. Materials with a low
thermal inertia, such as dust and other fine grained materials, quickly respond to
temperature changes, which results in a large temperature amplitude during a complete
lunar cycle. Surfaces covered with high thermal inertia materials, e.g., rocks or
bedrock, take more time to heat up during the day and reradiate the heat during
night.
We derived maps of thermal inertia from LRO-Diviner nighttime temperature data [3].
This approach is similar to martian thermal inertia derivations, as described by Mellon et al.
(2000) and Putzig et al. (2005) [2, 4]. In addition to studying thermal inertia, we also
calculated the relative rock abundances of selected study areas; e.g., the Apollo and
Luna Landing Sites. Due to the relatively large footprints of remote sensing data,
anisothermal surfaces are observed within the field of view. Consequently, multiple
thermal inertia units having variable temperatures are merged to a single observed
temperature. However, because the brightness temperature is a function of wavelength, it
increases with decreasing wavelength. This nonlinearity of the Planck radiance can
be used to determine the rock concentration of the observed surfaces [e.g., 5-7].
Therefore, we used our model surface temperatures for different thermal inertia and rock
abundances and compared these results to the LRO-Diviner temperature data at distinct
wavelengths.
The areas investigated in this study are covered by units of low thermal inertia material
with low rock abundances ( |
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