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dc.contributor.authorGuimond, Claire Marie
dc.contributor.authorRudge, John F
dc.contributor.authorShorttle, Oliver
dc.date.accessioned2022-03-28T19:06:09Z
dc.date.available2022-03-28T19:06:09Z
dc.date.issued2022-03-01
dc.date.submitted2021-10-08
dc.identifier.otherpsjac562e
dc.identifier.otherac562e
dc.identifier.otheraas35289
dc.identifier.urihttps://www.repository.cam.ac.uk/handle/1810/335407
dc.description.abstract<jats:title>Abstract</jats:title> <jats:p>Topography on a wet rocky exoplanet could raise land above its sea level. Although land elevation is the product of many complex processes, the large-scale topographic features on any geodynamically active planet are the expression of the convecting mantle beneath the surface. This so-called “dynamic topography” exists regardless of a planet’s tectonic regime or volcanism; its amplitude, with a few assumptions, can be estimated via numerical simulations of convection as a function of the mantle Rayleigh number. We develop new scaling relationships for dynamic topography on stagnant lid planets using 2D convection models with temperature-dependent viscosity. These scalings are applied to 1D thermal history models to explore how dynamic topography varies with exoplanetary observables over a wide parameter space. Dynamic topography amplitudes are converted to an ocean basin capacity, the minimum water volume required to flood the entire surface. Basin capacity increases less steeply with planet mass than does the amount of water itself, assuming a water inventory that is a constant planetary mass fraction. We find that dynamically supported topography alone could be sufficient to maintain subaerial land on Earth-size stagnant lid planets with surface water inventories of up to approximately 10<jats:sup>−4</jats:sup> times their mass, in the most favorable thermal states. By considering only dynamic topography, which has ∼1 km amplitudes on Earth, these results represent a lower limit to the true ocean basin capacity. Our work indicates that deterministic geophysical modeling could inform the variability of land propensity on low-mass planets.</jats:p>
dc.description.sponsorshipUniversity of Cambridge Harding Distinguished Postgraduate Scholars Programme and the Natural Sciences and Engineering Research Council of Canada (NSERC).
dc.languageen
dc.publisherAmerican Astronomical Society
dc.subject500
dc.subjectPlanetary Science
dc.titleBlue Marble, Stagnant Lid: Could Dynamic Topography Avert a Waterworld?
dc.typeArticle
dc.date.updated2022-03-28T19:06:09Z
prism.issueIdentifier3
prism.publicationNameThe Planetary Science Journal
prism.volume3
dc.identifier.doi10.17863/CAM.82836
dcterms.dateAccepted2022-02-15
rioxxterms.versionofrecord10.3847/psj/ac562e
rioxxterms.versionVoR
rioxxterms.licenseref.urihttp://creativecommons.org/licenses/by/4.0/
dc.contributor.orcidGuimond, Claire [0000-0003-1521-5461]
dc.contributor.orcidRudge, John [0000-0002-9399-7166]
dc.contributor.orcidShorttle, Oliver [0000-0002-8713-1446]
dc.identifier.eissn2632-3338
pubs.funder-project-idCambridge Trust (Cambridge Commonwealth, European & International Trust) (KFLS)
pubs.funder-project-idGouvernement du Canada ∣ Natural Sciences and Engineering Research Council of Canada (NSERC) (CGSD3-545674-2020)
cam.issuedOnline2022-03-25


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