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The widespread occurrence of high‐calcium pyroxene in bright‐ray craters on the Moon and implications for lunar‐crust composition
Author(s) -
Ogawa Y.,
Matsunaga T.,
Nakamura R.,
Saiki K.,
Ohtake M.,
Hiroi T.,
Takeda H.,
Arai T.,
Yokota Y.,
Yamamoto S.,
Hirata N.,
Sugihara T.,
Sasaki S.,
Haruyama J.,
Morota T.,
Honda C.,
Demura H.,
Kitazato K.,
Terazono J.,
Asada N.
Publication year - 2011
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2011gl048569
Subject(s) - impact crater , mafic , pyroxene , crust , geology , plagioclase , spectral line , absorption (acoustics) , geochemistry , mineral , mineralogy , astrobiology , olivine , astronomy , chemistry , quartz , physics , paleontology , optics , organic chemistry
We investigated the continuous spectral features of fresh craters on the Moon accompanied by distinctive bright rays, with cavity diameters between 8 and 24 km. We used the data from the Spectral Profiler onboard SELENE (Kaguya) to gain a better understanding of the composition of the lunar highland crust. We found that the observed spectra exhibited strong symmetric absorption around 1 μ m and recognizable absorption around 1.3 μ m. The spectra around a few craters showed a drastic change in the relative strengths of these two absorption bands s 1.3/1.0 at different locations in and around the craters, indicating differences in the abundance of plagioclase and mafic minerals. In contrast, the spectra around most of the craters showed no significant variation in spectral shape, with an essentially constant s 1.3/1.0 . We analyzed the absorption features of the craters with an essentially constant s 1.3/1.0 using the Modified Gaussian Model. We found that the strongest symmetric absorption bands were centered at 0.97–1.01 μ m with s 1.3/1.0 ≈ 0.2–0.6. Comparing these values with data from known samples, we concluded that high‐calcium pyroxene (HCP) is the most plausible dominant mafic mineral identified from the observed spectra. The fact that we detected such HCP‐dominant spectra among rayed craters widely spaced across the lunar highland implies that the major mafic component of some portions of the lunar crust is HCP rather than low‐calcium pyroxene (LCP).