@inproceedings{oai:jaxa.repo.nii.ac.jp:00020689,
 author = {斎藤, 靖之 and 疋田, 肇 and 横田, 康弘 and 白石, 浩章 and 田中, 智 and 水谷, 仁 and Saito, Yasuyuki and Hikida, Hajime and Yokota, Yasuhiro and Shiraishi, Hiroaki and Tanaka, Satoshi and Mizutani, Hitoshi},
 book = {第36回月・惑星シンポジウム, Proceedings of the 36th ISAS Lunar and Planetary Symposium},
 month = {Nov},
 note = {The past studies showed that surface heat, flow of the Moon obtained by the Apollo missions, does not, properly represent the regional averages due to a heat-flow focusing effect of the megaregolith, however the past studies used unrealistic models, in megaregolith thickness varied stepwise at the Apollo 15 or 17 site, and topographic variation is not considered. Re-examined was the effect of lateral heterogeneity of the megaregolith thickness and topography on the surface heat flow at Apollo 15 and 17 sites. The present numerical calculations indicate that the megaregolith and topographic effects on the heat flow amount to 10 to 50 percent of the observed heat flows. Correcting these effects, the abundance of the heat-generating elements in the crust can be estimated. A model with 40 times higher spatial resolution than past models was used in order to reexamine those effects. As a result, the value of skin depth D, which implies degree of upper concentration of the incompatible elements, is found to be significantly 20 to 30 km which is larger than that, on the earth, D = 10km. The large D value may suggest that the lunar magma, ocean generated lunar crust in large quantities in a short time., 資料番号: AA0046650040},
 pages = {157--160},
 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 = {Re-analysis of the lunar heat flow},
 year = {2003}
}