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dc.contributor.authorMayne, NJ
dc.contributor.authorDrummond, B
dc.contributor.authorDebras, F
dc.contributor.authorJaupart, E
dc.contributor.authorManners, J
dc.contributor.authorBoutle, I
dc.contributor.authorBaraffe, I
dc.contributor.authorKohary, K
dc.date.accessioned2018-12-10T15:16:45Z
dc.date.issued2019-01-22
dc.description.abstractWe present significant differences in the simulated atmospheric flow for warm, tidally-locked small Neptunes and super Earths (based on a nominal GJ 1214b) when solving the simplified, and commonly used, primitive dynamical equations or the full Navier-Stokes equations. The dominant prograde, superrotating zonal jet is markedly different between the simulations which are performed using practically identical numerical setups, within the same model. The differences arise due to the breakdown of the so-called `shallow-fluid' and traditional approximations, which worsens when rotation rates are slowed, and day{night temperature contrasts are increased. The changes in the zonal advection between simulations solving the full and simplified equations, give rise to significant differences in the atmospheric redistribution of heat, altering the position of the hottest part of the atmosphere and temperature contrast between the day and night sides. The implications for the atmospheric chemistry and, therefore, observations need to be studied with a model including a more detailed treatment of the radiative transfer and chemistry. Small Neptunes and super Earths are extremely abundant and important, potentially bridging the structural properties (mass, radius, composition) of terrestrial and gas giant planets. Our results indicate care is required when interpreting the output of models solving the primitive equations of motion for such planets.en_GB
dc.description.sponsorshipLeverhulme Trusten_GB
dc.description.sponsorshipScience and Technology Facilities Councilen_GB
dc.description.sponsorshipEuropean Research Councilen_GB
dc.identifier.citationVol. 871 (1). Published online 22 January 2019.en_GB
dc.identifier.doi10.3847/1538-4357/aaf6e9
dc.identifier.grantnumberRPG-2015-145en_GB
dc.identifier.grantnumberST/R000395/1en_GB
dc.identifier.grantnumber336792en_GB
dc.identifier.urihttp://hdl.handle.net/10871/35082
dc.language.isoenen_GB
dc.publisherAmerican Astronomical Society / IOP Publishingen_GB
dc.relation.urlhttps://doi.org/10.24378/exe.1023en_GB
dc.rights© 2019. The American Astronomical Society. All rights reserved.
dc.subjecteditorials, noticesen_GB
dc.subjectcataloguesen_GB
dc.subjectsurveysen_GB
dc.titleThe Limits of the Primitive Equations of Dynamics for Warm, Slowly Rotating Small Neptunes and Super Earths (article)en_GB
dc.typeArticleen_GB
dc.date.available2018-12-10T15:16:45Z
dc.identifier.issn1538-4357
dc.descriptionThis is the author accepted manuscript. The final version is available from American Astronomical Society / IOP Publishing via the DOI in this record.en_GB
dc.descriptionThe dataset associated with this article is located in ORE at: https://doi.org/10.24378/exe.1023en_GB
dc.identifier.journalAstrophysical Journalen_GB
dc.rights.urihttp://www.rioxx.net/licenses/all-rights-reserveden_GB
dcterms.dateAccepted2018-12-07
exeter.funder::Leverhulme Trusten_GB
exeter.funder::Science and Technology Facilities Councilen_GB
rioxxterms.versionAMen_GB
rioxxterms.licenseref.startdate2018-12-07
rioxxterms.typeJournal Article/Reviewen_GB
refterms.dateFCD2018-12-10T10:44:12Z
refterms.versionFCDAM
refterms.dateFOA2019-01-23T15:10:20Z
refterms.panelBen_GB


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