Show simple item record

dc.contributor.authorChan, N.-H.
dc.contributor.authorMitrovica, Jerry
dc.contributor.authorDaradich, A.
dc.contributor.authorCreveling, J. R.
dc.contributor.authorMatsuyama, I.
dc.contributor.authorStanley, S.
dc.date.accessioned2019-09-25T17:53:59Z
dc.date.issued2014
dc.identifier.citationChan, N.-H., J. X. Mitrovica, A. Daradich, J. R. Creveling, I. Matsuyama, and S. Stanley. 2014. “Time-Dependent Rotational Stability of Dynamic Planets with Elastic Lithospheres.” Journal of Geophysical Research: Planets 119 (1): 169–88. https://doi.org/10.1002/2013je004466.
dc.identifier.issn2169-9097
dc.identifier.issn2169-9100
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41401427*
dc.description.abstractTrue polar wander (TPW), a reorientation of the rotation axis relative to the solid body, is driven by mass redistribution on the surface or within the planet and is stabilized by two aspects of the planet's viscoelastic response: the delayed viscous readjustment of the rotational bulge and the elastic stresses in the lithosphere. The latter, following Willemann (1984), is known as remnant bulge stabilization. In the absence of a remnant bulge, the rotation of a terrestrial planet is said to be inherently unstable. Theoretical treatments have been developed to treat the final (equilibrium) state in this case and the time-dependent TPW toward this state, including nonlinear approaches that assume slow changes in the inertia tensor. Moreover, remnant bulge stabilization has been incorporated into both equilibrium and linearized, time-dependent treatments of rotational stability. We extend the work of Ricard et al. (1993) to derive a nonlinear, time-dependent theory of TPW that incorporates stabilization by both the remnant bulge and viscous readjustment of the rotational bulge. We illustrate the theory using idealized surface loading scenarios applied to models of both Earth and Mars. We demonstrate that the inclusion of remnant bulge stabilization reduces both the amplitude and timescale of TPW relative to calculations in which this stabilization is omitted. Furthermore, given current estimates of mantle viscosity for both planets, our calculations indicate that departures from the equilibrium orientation of the rotation axis in response to forcings with timescale of 1 Myr or greater are significant for Earth but negligible for Mars.
dc.language.isoen_US
dc.publisherAmerican Geophysical Union
dash.licenseLAA
dc.titleTime-dependent rotational stability of dynamic planets with elastic lithospheres
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalJournal of Geophysical Research - Planets
dash.depositing.authorMitrovica, Jerry
dc.date.available2019-09-25T17:53:59Z
dash.workflow.comments1Science Serial ID 47265
dc.identifier.doi10.1002/2013JE004466
dash.source.volume119;1
dash.source.page169-188
dash.contributor.affiliatedMitrovica, Jerry


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record