@inproceedings{oai:jaxa.repo.nii.ac.jp:00020424,
 author = {山本, 拓 and 大竹, 真紀子 and 岩田, 隆浩 and Yamamoto, Taku and Otake, Makiko and Iwata, Takahiro},
 book = {第40回月・惑星シンポジウム, Proceedings of the 40th ISAS Lunar and Planetary Symposium},
 month = {Jul},
 note = {The TiO2 distribution of the lunar surface helps us to understand the lunar igneous evolution processes. Ilmenite is the dominant carrier of the titanium on the lunar surface. Therefore, the lunar surface TiO2 map has been made by several scientists (Lucey et al., 1998, 2000) basically using the characteristics of the ilmenite spectrum, which is dark from 300 nm to 2,600 nm wavelength region and the reflectance at 415 nm and 750 nm are flat. But, past methods are probably not enough to estimate accurately the lunar surface TiO2 abundance, because the effect of existence of the absorption around 500 nm and grain size variation within lunar regolith on the estimation method of the TiO2 (ilmenite) abundance are not evaluated. In this work, we measured the ilmenite reflectance spectra of different grain size and estimated the grain size effect on the reflectance spectra to evaluate the estimation method of the TiO2 abundance. As a result, we haven't found the clear ilmenite absorption band around 500 nm at visible wavelength which is reported previously (Holsclaw et al., 2005) and the reflectance spectra are darker in smaller grain size measurements. These results indicated that we might be able to establish the new estimation method of the TiO2 abundance on the lunar surface by evaluating grain size effect on the reflectance spectra., 資料番号: AA0063723004},
 pages = {12--18},
 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 = {Estimation method of the TiO2 (ilmenite) abundance of the lunar surface using UVVIS reflectance spectra regarding the effect of the grain size},
 year = {2007}
}