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Styles of mantle convection and their influence on planetary evolution

Stevenson, David J. (2003) Styles of mantle convection and their influence on planetary evolution. Comptes Rendus Geoscience, 335 (1). pp. 99-111. ISSN 1631-0713. https://resolver.caltech.edu/CaltechAUTHORS:20130730-110406267

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Abstract

Mantle convection is the method of heat elimination for silicate mantles in terrestrial bodies, provided they are not too small or too hot. Bodies that are small (∼Moon or smaller, possibly even Mercury) may rely largely on conduction or melt migration, and bodies that are very hot (Io, very early Earth) may use massive melt migration (magma oceans) and heat pipes. In the standard, simple picture, we can use scaling laws to determine the secular cooling of a planet, likelihood and form of volcanism, and the possibility of a core dynamo. Contrary to popular belief, small planets do not cool faster than larger planets (provided they convect) but they do tend to have a slightly lower internal temperature at all times and thus may cease to be volcanically active at an earlier epoch. On the other hand, a larger volume fraction of a small planet may be involved in melt generation. However, our understanding of heat transfer by mantle convection is limited by three very important, largely unsolved problems: The complexities of rheology, the effects of compositional gradients, and the effects of phase transitions, especially melting. The most striking manifestation of the role of rheology lies in the difference between a mobile lid mode (plate tectonics for Earth) and a stagnant lid mode (other large terrestrial bodies). This difference may arise because of the role of water, but perhaps also because of melting, or size (gravity), or the vagaries of history. It has profound effects for the differences in history of Earth, Venus and Mars, including their surface geology, volatile reservoirs and magnetic fields. Since thermal convection is driven by small density differences, it can also be greatly altered or limited by compositional or phase effects. Melt migration introduces additional complications to the heat transport as well as being a source for the irreversible differentiation that might promote layering. Our limited understanding and ability to model these processes continues to limit the development of a predictive framework for the differences among the terrestrial planets.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1016/S1631-0713(03)00009-9DOIArticle
http://www.sciencedirect.com/science/article/pii/S1631071303000099PublisherArticle
ORCID:
AuthorORCID
Stevenson, David J.0000-0001-9432-7159
Alternate Title:Les styles de convection du manteau et leur influence sur l'évolution des planètes
Additional Information:© 2003 Académie des sciences/Éditions scientifiques et médicales Elsevier SAS. Received 17 July 2002; accepted 7 November 2002. Written on invitation of the Editorial Board. Thanks to reviewers A. Davaille and N. Sleep for useful comments. Work supported by NASA Geology and Geophysics program.
Funders:
Funding AgencyGrant Number
NASAUNSPECIFIED
Subject Keywords:Mantle convection; Planetary evolution; Convection du manteau; Évolution des planètes
Issue or Number:1
Record Number:CaltechAUTHORS:20130730-110406267
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20130730-110406267
Official Citation:David J. Stevenson, Styles of mantle convection and their influence on planetary evolution, Comptes Rendus Geoscience, Volume 335, Issue 1, January 2003, Pages 99-111, ISSN 1631-0713, http://dx.doi.org/10.1016/S1631-0713(03)00009-9.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:39654
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:19 Aug 2013 22:12
Last Modified:03 Oct 2019 05:09

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