| Project/Area Number |
20244073
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| Research Category |
Grant-in-Aid for Scientific Research (A)
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| Allocation Type | Single-year Grants |
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| Section | 一般 |
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| Research Field |
Solid earth and planetary physics
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| Research Institution | National Astronomical Observatory of Japan |
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Principal Investigator |
SASAKI Sho 国立天文台, RISE月探査プロジェクト, 教授 (10183823)
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| Co-Investigator(Kenkyū-buntansha) |
HANADA Hideo 国立天文台, RISE月探査プロジェクト, 准教授 (60132677)
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| Co-Investigator(Renkei-kenkyūsha) |
ARAKI Hiroshi 国立天文台, RISE月探査プロジェクト, 助教 (10290884)
MATSUMOTO Koji 国立天文台, RISE月探査プロジェクト, 准教授 (30332167)
NODA Hirotomo 国立天文台, RISE月探査プロジェクト, 助教 (10353426)
KAWANO Nobuyuki 国立天文台, RISE月探査プロジェクト, 名誉教授 (10186116)
IWATA Takahiro 独立行政法人宇宙航空研究開発機構, 宇宙科学研究本部, 准教授 (20201949)
HARUYAMA Junichi 独立行政法人宇宙航空研究開発機構, 宇宙科学研究本部, 助教 (40373443)
OTAKE Makiko 独立行政法人宇宙航空研究開発機構, 宇宙科学研究本部, 助教 (30373442)
MATSUNAGA Tsuneo 独立行政法人国立環境研究所, 地球環境研究センター, 室長 (70302966)
NAMIKI Noriyuki 千葉工業大学, 惑星探査センター, 副所長 (50274428)
DEMURA Hirohide 会津大学, コンピュータ理工学部, 准教授 (10360009)
YAMAGUCHI Yasushi 名古屋大学, 環境学研究科, 教授 (80283472)
YAMAJI Atsushi 京都大学, 理学研究科, 教授 (40212287)
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| Project Period (FY) |
2008 – 2011
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| Project Status |
Completed (Fiscal Year 2011)
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| Budget Amount *help |
¥47,580,000 (Direct Cost: ¥36,600,000、Indirect Cost: ¥10,980,000)
Fiscal Year 2011: ¥6,630,000 (Direct Cost: ¥5,100,000、Indirect Cost: ¥1,530,000)
Fiscal Year 2010: ¥10,010,000 (Direct Cost: ¥7,700,000、Indirect Cost: ¥2,310,000)
Fiscal Year 2009: ¥10,790,000 (Direct Cost: ¥8,300,000、Indirect Cost: ¥2,490,000)
Fiscal Year 2008: ¥20,150,000 (Direct Cost: ¥15,500,000、Indirect Cost: ¥4,650,000)
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| Keywords | 月 / 重力 / 内部構造 / 二分性 / 地殻 / かぐや / 衝突盆地 / VLBI / 重力場 / VLBIss |
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| Research Abstract |
In JAXA KAGUYA(SELENE) mission, using two subsatellites and VLBI observations by VERA 4 stations and international 4 stations, the first global accurate gravitational field of the Moon including the far-side was obtained. The first global accurate lunar topography was also obtained by a laser altimeter. Multi-frequency differential VLBI was proven to be the powerful technique for orbital determination(less than 1cm, 1mm in principle). Global distribution of lunar crust was obtained from gravity and topography data. The thinnest crust was beneath Mare Moscoviences on the far-side. 500-1000km scale far-side highland impact structures are supported mostly by the crust which would have been cooled faster than near-side crust.
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