Structure of lunar crust from KAGUYA selenodesy data

Details Structure of lunar crust from KAGUYA selenodesy data Structure of lunar crust from KAGUYA selenodesy data

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1073s&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1073

Physics

Scientific paper

Using 4-way Doppler tracking with relay satellite OKINA, KAGUYA obtained the first precise gravity field of the lunar farside. Multi-frequency differential VLBI observation of subsatellites OKINA and OUNA improved the accuracy of gravity. KAGUYA also has a laser altimeter (LALT) which obtained the first global topography of the moon including polar regions. Assuming uniform crustal density, we obtain crustal thickness distribution where crustal thickness is nearly zero beneath Mare Moscoviense. The interior structure of the South Pole-Aitken basin (SPA) is investigated using localized representation of gravity potential where Slepian functions were used to estimate the gravity field over certain areas of the Moon. The direction of an ellipse denoting the depression is similar to the previous result. The region with the thinnest crust is nearly circular and offset southward from the center of SPA. We analyzed interior structure of small basins in and around SPA.

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