Other
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p41b1619h&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P41B-1619
Other
[1221] Geodesy And Gravity / Lunar And Planetary Geodesy And Gravity, [5430] Planetary Sciences: Solid Surface Planets / Interiors, [5450] Planetary Sciences: Solid Surface Planets / Orbital And Rotational Dynamics, [5455] Planetary Sciences: Solid Surface Planets / Origin And Evolution
Scientific paper
In the present study, temporal variation of a paleo-pole position due to TPW is formulated and calculated based on strain energy in a previous study. Especially, quasi-fluid approximation is suitable to deal with large-scale and long-term variation of a paleo-pole position. Thus, an orientation of a paleo-rotation axis in each time step is estimated in here by following conventional formulation with the quasi-fluid approximation for TPW, and simultaneously by taking total energy minimization into account. In practice, this procedure is physically same as to incorporate elastic torque due to tidal deformation of a lithosphere into the Liouville equation including the quasi-fluid approximation. In this study, like the previous one, only one symmetric surface load is regarded as a driving force of TPW for convenience sake. In this calculation, variable parameters are defined as follows: a location of emplacement, duration of formation, and maximum of intensity of a load. The result with strain energy is compared with that without strain energy. As a result, the case with the strain energy indicates different characteristics from that without the strain energy in the following points. First, the paleo-poles under steady states are different each other in the cases for same parameters. These results are not consistent even with the previous results concerning just the final condition. Second, also in the cases for same parameters, time scales when the paleo-poles reach the static limits are different. These results demonstrate the fact that strain energy within a lithosphere effectively weakens influence of a load on TPW. Although this kind of influence has already been pointed out by the previous results just in the cases of the steady states, the present results further revealed similar effect also on a characteristic time scale of TPW. Strictly speaking, however, it is impossible to estimate this exact time scale only by reducing an effective size of a load. This is because it is possible that secular variation in strain energy induced by TPW occurs also after formation of a load itself as driving force. This delay results from visco-elastic readjustment of centrifugal bulge in response to long-term polar motion. In conclusion, the present results imply that strain energy is not necessarily negligible in terms of physical interpretation for realistic TPW, especially characteristic time scales and time variations between the initial and final states of the spin axis.
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