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  • 11
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    Annealing effects on the ferromagnetic resonance linewidths of sputter-deposited Fe100−xCox(001) thin films (x  (2015)
    American Institute of Physics (AIP)
    Details
    Publication Date: 2015-04-07
    Description: Effects of post-growth annealing on the magnetic damping of 3d transition alloy thin films were investigated. Fe 100−x Co x (x 
    Print ISSN: 0021-8979
    Electronic ISSN: 1089-7550
    Topics: Physics
    Published by American Institute of Physics (AIP)
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  • 12
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    Massive layer of pure anorthosite on the Moon (2012)
    Wiley
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    Publication Date: 2012-07-06
    Description: We present a new global survey of the purest anorthosite (PAN) rock using the Spectral Profiler onboard Kaguya. We found that PAN rocks are widely distributed over the Moon, including the Feldspathic Highland Terrain and the south and north polar regions. All PAN sites are associated with huge impact structures with diameters larger than 100 km. Based on the global distributions of PAN and olivine-rich sites, we propose the existence of a massive PAN layer with a thickness of ∼50 km below an uppermost mafic-rich mixed layer with a thickness of ∼10 km. Below the PAN layer, a lower crustal layer with olivine-rich materials may be present on the nearside, but not on the far side of the Moon. The existence of a PAN layer with a thickness of ∼50 km suggests an Al2O3 abundance of 33 to 34 wt.% in the lunar crust, which is higher than previous estimates of
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 13
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    The widespread occurrence of high-calcium pyroxene in bright-ray craters on the Moon and implications for lunar-crust composition (2011)
    Wiley
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    Publication Date: 2011-09-08
    Description: 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 μm and recognizable absorption around 1.3 μm. The spectra around a few craters showed a drastic change in the relative strengths of these two absorption bands s1.3/1.0 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 s1.3/1.0. We analyzed the absorption features of the craters with an essentially constant s1.3/1.0 using the Modified Gaussian Model. We found that the strongest symmetric absorption bands were centered at 0.97–1.01 μm with s1.3/1.0 ≈ 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).
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 14
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    Thermal properties of methane hydrate bearing sediments and surrounding muds recovered from Nankai-Trough wells (2014)
    Wiley
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    Publication Date: 2014-10-29
    Description: ABSTRACT This paper presents the measurement of the thermal constants of natural methane-hydrate-bearing sediments and mud-layer samples recovered from wells. Core samples were recovered from the Tokai-oki test wells (Nankai-Trough, Japan) in 2004. The thermal conductivity, thermal diffusivity, and specific heat of the samples were simultaneously determined using the hot-disk transient method. The thermal conductivity of natural hydrate-bearing sediments decreased slightly with increasing porosity. In addition, the thermal diffusivity of hydrate-bearing sediments decreased as the porosity increased. Moreover, we also used simple models to calculate the thermal conductivity and diffusivity. Estimations of the distribution model (geometric-mean model) were relatively consistent with the measured results, suggesting that sand grains and hydrates should be independently distributed for hydrate-bearing sediments, which exhibit a pore-filling pattern. The measurement results were also consistent with the thermal diffusivity, which was estimated by dividing the thermal conductivity obtained from the distribution model by the specific heat taken from the arithmetic mean. Finally, our estimate of the thermal conductivity of silt soil was much lower than that for sand soil in hydrate-bearing sediment, which suggests that the small grains influence thermal conductivity.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 15
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    Global occurrence trend of high-Ca pyroxene on lunar highlands and its implications (2015)
    Wiley
    Details
    Publication Date: 2015-03-25
    Description: We present details of the global distribution of high-Ca pyroxene (HCP)-rich sites in the lunar highlands based on the global dataset of hyper-spectral reflectance obtained by the SELENE Spectral Profiler. Most HCP-rich sites in the lunar highlands are found at fresh impact craters. In each crater, most of the detection points are distributed on the ejecta, rim, and floor of the impact craters rather than the central peaks, while the central peaks are dominated by purest anorthosite (PAN). This indicates that HCP-rich materials originate from relatively shallower regions of the lunar crust than PAN. In addition, while all ray craters with sizes larger than ~40km possess HCP-rich materials, small fresh craters with sizes less than ~6−−10km do not, indicating that the uppermost mixing layers in the lunar crust are not dominated by HCP. Based on these results, we propose that in the upper lunar crust, a HCP-rich zone overlying the PAN layer exists below the uppermost mixing layer. This HCP-rich zone may originate from interstitial melt during the formation of the flotation anorthositic cumulate, while an impact ejecta origin, impact melt origin, and/or magmatic intrusion into the upper lunar crust may also account for the occurrence of HCP-rich sites in the highlands.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 16
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    Variation of the lunar highland surface roughness at baseline 0.15–100 km and the relationship to relative age (2014)
    Wiley
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    Publication Date: 2014-03-12
    Description: We report the surface roughness analysis of the lunar highlands for the baseline range 0.15–100 km. We use the Median Differential Slope α m to investigate the scale dependency of the roughness and derive the global α m distribution from SELENE Laser Altimeter and Terrain Camera data. While α m ( l ) versus baseline l (km) plots vary among different highland types, all highlands commonly show a peak at 3–30 km. The Pre-Nectarian surface shows a relatively large α m (20–30 km). Our analysis is supported by the simulation of synthetic surface cratering models and crater statistics. In our simulation, a peak of α m (30 km) is successfully reproduced. The actual crater density shows good correlation with an empirical roughness indicator. However, a large part of the Nectarian surface shows a peak at 6–9 km baseline. This peak may be caused by secondary craters and ejecta deposit textures from the Nectarian system basins.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 17
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    The global distribution of pure anorthosite on the Moon (2009)
    Nature Publishing Group (NPG)
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    Publication Date: 2009-09-11
    Description: It has been thought that the lunar highland crust was formed by the crystallization and floatation of plagioclase from a global magma ocean, although the actual generation mechanisms are still debated. The composition of the lunar highland crust is therefore important for understanding the formation of such a magma ocean and the subsequent evolution of the Moon. The Multiband Imager on the Selenological and Engineering Explorer (SELENE) has a high spatial resolution of optimized spectral coverage, which should allow a clear view of the composition of the lunar crust. Here we report the global distribution of rocks of high plagioclase abundance (approaching 100 vol.%), using an unambiguous plagioclase absorption band recorded by the SELENE Multiband Imager. If the upper crust indeed consists of nearly 100 vol.% plagioclase, this is significantly higher than previous estimates of 82-92 vol.% (refs 2, 6, 7), providing a valuable constraint on models of lunar magma ocean evolution.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Ohtake, Makiko -- Matsunaga, Tsuneo -- Haruyama, Junichi -- Yokota, Yasuhiro -- Morota, Tomokatsu -- Honda, Chikatoshi -- Ogawa, Yoshiko -- Torii, Masaya -- Miyamoto, Hideaki -- Arai, Tomoko -- Hirata, Naru -- Iwasaki, Akira -- Nakamura, Ryosuke -- Hiroi, Takahiro -- Sugihara, Takamitsu -- Takeda, Hiroshi -- Otake, Hisashi -- Pieters, Carle M -- Saiki, Kazuto -- Kitazato, Kohei -- Abe, Masanao -- Asada, Noriaki -- Demura, Hirohide -- Yamaguchi, Yasushi -- Sasaki, Sho -- Kodama, Shinsuke -- Terazono, Junya -- Shirao, Motomaro -- Yamaji, Atsushi -- Minami, Shigeyuki -- Akiyama, Hiroaki -- Josset, Jean-Luc -- England -- Nature. 2009 Sep 10;461(7261):236-40. doi: 10.1038/nature08317.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshino-dai, Sagamihara, Kanagawa 229-8510, Japan.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19741704" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 18
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    Lack of exposed ice inside lunar south pole Shackleton Crater (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-10-25
    Description: The inside of Shackleton Crater at the lunar south pole is permanently shadowed; it has been inferred to hold water-ice deposits. The Terrain Camera (TC), a 10-meter-resolution stereo camera onboard the Selenological and Engineering Explorer (SELENE) spacecraft, succeeded in imaging the inside of the crater, which was faintly lit by sunlight scattered from the upper inner wall near the rim. The estimated temperature of the crater floor, based on the crater shape model derived from the TC data, is less than approximately 90 kelvin, cold enough to hold water-ice. However, at the TC's spatial resolution, the derived albedo indicates that exposed relatively pure water-ice deposits are not on the crater floor. Water-ice may be disseminated and mixed with soil over a small percentage of the area or may not exist at all.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Haruyama, Junichi -- Ohtake, Makiko -- Matsunaga, Tsuneo -- Morota, Tomokatsu -- Honda, Chikatoshi -- Yokota, Yasuhiro -- Pieters, Carle M -- Hara, Seiichi -- Hioki, Kazuyuki -- Saiki, Kazuto -- Miyamoto, Hideaki -- Iwasaki, Akira -- Abe, Masanao -- Ogawa, Yoshiko -- Takeda, Hiroshi -- Shirao, Motomaro -- Yamaji, Atsushi -- Josset, Jean-Luc -- New York, N.Y. -- Science. 2008 Nov 7;322(5903):938-9. doi: 10.1126/science.1164020. Epub 2008 Oct 23.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-85105, Japan.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18948501" target="_blank"〉PubMed〈/a〉
    Keywords: Cold Temperature ; Extraterrestrial Environment ; *Ice ; *Moon ; Spacecraft
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 19
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    Long-lived volcanism on the lunar farside revealed by SELENE Terrain Camera (2008)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2008-11-08
    Description: We determined model ages of mare deposits on the farside of the Moon on the basis of the crater frequency distributions in 10-meter-resolution images obtained by the Terrain Camera on SELENE (Selenological and Engineering Explorer) (Kaguya). Most mare volcanism that formed mare deposits on the lunar farside ceased at approximately 3.0 billion years ago, suggesting that mare volcanism on the Moon was markedly reduced globally during this period. However, several mare deposits at various locations on the lunar farside also show a much younger age, clustering at approximately 2.5 billion years ago. These young ages indicate that mare volcanism on the lunar farside lasted longer than was previously considered and may have occurred episodically.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Haruyama, Junichi -- Ohtake, Makiko -- Matsunaga, Tsuneo -- Morota, Tomokatsu -- Honda, Chikatoshi -- Yokota, Yasuhiro -- Abe, Masanao -- Ogawa, Yoshiko -- Miyamoto, Hideaki -- Iwasaki, Akira -- Pieters, Carle M -- Asada, Noriaki -- Demura, Hirohide -- Hirata, Naru -- Terazono, Junya -- Sasaki, Sho -- Saiki, Kazuto -- Yamaji, Atsushi -- Torii, Masaya -- Josset, Jean-Luc -- New York, N.Y. -- Science. 2009 Feb 13;323(5916):905-8. doi: 10.1126/science.1163382. Epub 2008 Nov 6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshino-dai, Sagamihara, Kanagawa 229-8510, Japan. haruyama.junichi@jaxa.jp〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18988811" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 20
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    A new type of pyroclastic deposit on the Moon containing Fe-spinel and chromite (2013)
    Wiley
    Details
    Publication Date: 2013-07-26
    Description: [1]  We present details of the identification of sites that show an absorption band at visible wavelengths and a strong 2  μ m band using the SELENE Spectral Profiler. All the sites exhibiting the visible feature are found on the regional dark mantle deposit (DMD) at Sinus Aestuum. All the instances of the visible feature show a strong 2- μ m band, suggestive of Fe- and Cr-rich spinels, which are different from previously-detected Mg-rich spinel. Since no visible feature is observed in other DMDs, the DMD at Sinus Aestuum is unique on the Moon. The occurrence trend of the spinels at Sinus Aestuum is also different from that of the Mg-rich spinels, which are associated with impact structures. This may suggest that the spinel at Sinus Aestuum is a different origin from that of the Mg-rich spinel.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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