HR: 15:25h
AN: G33A-08    [Abstracts]
TI: Lunar Rotation, Orientation and Science
AU: Williams, J G
EM: James.G.Williams@jpl.nasa.gov
AF: Jet Propulsion Laboratory, MS 238-332, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: * Ratcliff, J T
EM: J.Todd.Ratcliff@jpl.nasa.gov
AF: Jet Propulsion Laboratory, MS 238-332, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AU: Boggs, D H
EM: Dale.H.Boggs@jpl.nasa.gov
AF: Jet Propulsion Laboratory, MS 238-332, 4800 Oak Grove Dr., Pasadena, CA 91109 United States
AB: The Moon is the most familiar example of the many satellites that exhibit synchronous rotation. For the Moon there is Lunar Laser Ranging measurements of tides and three-dimensional rotation variations plus supporting theoretical understanding of both effects. Compared to uniform rotation and precession the lunar rotational variations are up to 1 km, while tidal variations are about 0.1 m. Analysis of the lunar variations in pole direction and rotation about the pole gives moment of inertia differences, third-degree gravity harmonics, tidal Love number k$_{2}$, tidal dissipation Q vs. frequency, dissipation at the fluid-core/solid-mantle boundary, and emerging evidence for an oblate boundary. The last two indicate a fluid core, but a solid inner core is not ruled out. Four retroreflectors provide very accurate positions on the Moon. The experience with the Moon is a starting point for exploring the tides, rotation and orientation of the other synchronous bodies of the solar system.
DE: 6250 Moon (1221)
DE: 1221 Lunar geodesy and gravity (6250)
SC: Geodesy [G]
MN: 2004 AGU Fall Meeting