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dc.contributor.authorHeap, Michael J.
dc.contributor.authorByrne, Paul K.
dc.contributor.authorMikhail, Sami
dc.identifier.citationHeap , M J , Byrne , P K & Mikhail , S 2017 , ' Low surface gravitational acceleration of Mars results in a thick and weak lithosphere : implications for topography, volcanism, and hydrology ' , Icarus , vol. 281 , pp. 103-114 .
dc.identifier.otherPURE: 245703156
dc.identifier.otherPURE UUID: 105a52ec-6eee-4d36-b74b-f6c015773585
dc.identifier.otherScopus: 84991705015
dc.identifier.otherORCID: /0000-0001-5276-0229/work/37274386
dc.identifier.otherWOS: 000385478100008
dc.descriptionThe first author acknowledges funding from an Initiative d’Excellence (IDEX) “Attractivité” grant (VOLPERM), funded by the University of Strasbourg. M.H. also acknowledges support from the CNRS (INSU 2016-TelluS-ALEAS).en
dc.description.abstractSurface gravitational acceleration (surface gravity) on Mars, the second-smallest planet in the Solar System, is much lower than that on Earth. A direct consequence of this low surface gravity is that lithostatic pressure is lower on Mars than on Earth at any given depth. Collated published data from deformation experiments on basalts suggest that, throughout its geological history (and thus thermal evolution), the Martian brittle lithosphere was much thicker but weaker than that of present-day Earth as a function solely of surface gravity. We also demonstrate, again as a consequence of its lower surface gravity, that the Martian lithosphere is more porous, that fractures on Mars remain open to greater depths and are wider at a given depth, and that the maximum penetration depth for opening-mode fractures (i.e., joints) is much deeper on Mars than on Earth. The result of a weak Martian lithosphere is that dykes—the primary mechanism for magma transport on both planets—can propagate more easily and can be much wider on Mars than on Earth. We suggest that this increased the efficiency of magma delivery to and towards the Martian surface during its volcanically active past, and therefore assisted the exogeneous and endogenous growth of the planet's enormous volcanoes (the heights of which are supported by the thick Martian lithosphere) as well as extensive flood-mode volcanism. The porous and pervasively fractured (and permeable) nature of the Martian lithosphere will have also greatly assisted the subsurface storage of and transport of fluids through the lithosphere throughout its geologically history. And so it is that surface gravity, influenced by the mass of a planetary body, can greatly modify the mechanical and hydraulic behaviour of its lithosphere with manifest differences in surface topography and geomorphology, volcanic character, and hydrology.
dc.rights© 2016 Published by Elsevier Inc. This work is made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at
dc.subjectG Geography (General)en
dc.subjectQB Astronomyen
dc.titleLow surface gravitational acceleration of Mars results in a thick and weak lithosphere : implications for topography, volcanism, and hydrologyen
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews. School of Earth & Environmental Sciencesen
dc.contributor.institutionUniversity of St Andrews. St Andrews Isotope Geochemistryen
dc.contributor.institutionUniversity of St Andrews. Earth and Environmental Sciencesen
dc.description.statusPeer revieweden

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