HR: 0800h
AN: G51A-0804    [Abstracts]
TI: Secular Obliquity Variations Due to Climate Friction on Mars: Re-examination in Influence of Martian Internal Viscosity Structure
AU: * Harada, Y
EM: harada@miz.nao.ac.jp
AF: Division of Earth Mechanics, Earthquake Research Institute, the University of Tokyo, 1-1-1 Yayoi, Bunkyo, Tokyo, 113-0032 Japan
AU: * Harada, Y
EM: harada@miz.nao.ac.jp
AF: Mizusawa Astrogeodynamics Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-12 Hoshigaoka, Mizusawa, Iwate, 023-0861 Japan
AU: Heki, K
EM: heki@ep.sci.hokudai.ac.jp
AF: Division of Earth and Planetary Sciences, Graduate School of Science, Hokkaido University, 8 Nishi, 10 Kita, Kita, Sapporo, Hokkaido, 060-0810 Japan
AB: Secular obliquity variations due to climate friction on Mars are calculated. Martian interior is considered to be a three-layered structure. A viscosity of each layer is treated as a parameter. The results give knowledge as follows. First, under an internal structure with a crust of ``finite viscosity'' and/or a ``solid'' core, the effect of the climate friction becomes greater than that concluded by previous research. Second, under an internal structure with a mantle of ``heterogeneous viscosity'' the possibility of the great effect of the climate friction becomes stronger than that concluded by previous research.
DE: 0726 Ice sheets
DE: 1236 Rheology of the lithosphere and mantle (7218, 8160)
DE: 1621 Cryospheric change (0776)
DE: 5450 Orbital and rotational dynamics (1221)
DE: 6225 Mars
SC: Geodesy [G]
MN: Fall Meeting 2005