@inproceedings{oai:jaxa.repo.nii.ac.jp:00020479,
 author = {丸山, 陽子 and 白井, 慶 and 山本, 幸生 and 岡田, 達明 and 加藤, 學 and Maruyama, Yoko and Shirai, Kei and Yamamoto, Yukio and Okada, Tatsuaki and Kato, Manabu},
 book = {第39回月・惑星シンポジウム, Proceedings of the 39th ISAS Lunar and Planetary Symposium},
 month = {Aug},
 note = {Planetary surfaces are usually covered with regolith, which is far from ideal for detailed X-ray fluorescence analysis because its powdery rough surface affects XRF (X-Ray Fluorescence) intensities. Kuwada et al. (1997) pointed out this phenomenon could cause a serious error in determining rock-types, particularly observed at large phase angles. We measured XRF intensities for crashed rock samples in various grain sizes and investigated the angular dependency. Our results indicate that (1) XRF intensity decreases with increase in particle size, and its trend is more remarkable for lighter elements; (2) XRF normal to the surface is more intense for the lighter elements at the larger incident angles; (3) grain size effect seems more remarkable at larger phase angles; (4) XRF intensities should be corrected at grain size over 35 microns for Si and Ca, and over 67.5-135 microns for Fe under this experimental configuration. These results can support the shadowing and shading effects caused by microscopic roughness of powdery surface., 資料番号: AA0063505017},
 pages = {65--68},
 publisher = {宇宙航空研究開発機構宇宙科学研究本部, Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA/ISAS)},
 title = {Laboratory experiments of X-ray fluorescence intensity by simulating lunar and planetary rough surfaces},
 year = {2006}
}