dc.contributor.author | Mayne, NJ | |
dc.contributor.author | Drummond, B | |
dc.contributor.author | Debras, F | |
dc.contributor.author | Jaupart, E | |
dc.contributor.author | Manners, J | |
dc.contributor.author | Boutle, I | |
dc.contributor.author | Baraffe, I | |
dc.contributor.author | Kohary, K | |
dc.date.accessioned | 2018-12-10T15:16:45Z | |
dc.date.issued | 2019-01-22 | |
dc.description.abstract | We 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.sponsorship | Leverhulme Trust | en_GB |
dc.description.sponsorship | Science and Technology Facilities Council | en_GB |
dc.description.sponsorship | European Research Council | en_GB |
dc.identifier.citation | Vol. 871 (1). Published online 22 January 2019. | en_GB |
dc.identifier.doi | 10.3847/1538-4357/aaf6e9 | |
dc.identifier.grantnumber | RPG-2015-145 | en_GB |
dc.identifier.grantnumber | ST/R000395/1 | en_GB |
dc.identifier.grantnumber | 336792 | en_GB |
dc.identifier.uri | http://hdl.handle.net/10871/35082 | |
dc.language.iso | en | en_GB |
dc.publisher | American Astronomical Society / IOP Publishing | en_GB |
dc.relation.url | https://doi.org/10.24378/exe.1023 | en_GB |
dc.rights | © 2019. The American Astronomical Society. All rights reserved. | |
dc.subject | editorials, notices | en_GB |
dc.subject | catalogues | en_GB |
dc.subject | surveys | en_GB |
dc.title | The Limits of the Primitive Equations of Dynamics for Warm, Slowly Rotating Small Neptunes and Super Earths (article) | en_GB |
dc.type | Article | en_GB |
dc.date.available | 2018-12-10T15:16:45Z | |
dc.identifier.issn | 1538-4357 | |
dc.description | This 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.description | The dataset associated with this article is located in ORE at: https://doi.org/10.24378/exe.1023 | en_GB |
dc.identifier.journal | Astrophysical Journal | en_GB |
dc.rights.uri | http://www.rioxx.net/licenses/all-rights-reserved | en_GB |
dcterms.dateAccepted | 2018-12-07 | |
exeter.funder | ::Leverhulme Trust | en_GB |
exeter.funder | ::Science and Technology Facilities Council | en_GB |
rioxxterms.version | AM | en_GB |
rioxxterms.licenseref.startdate | 2018-12-07 | |
rioxxterms.type | Journal Article/Review | en_GB |
refterms.dateFCD | 2018-12-10T10:44:12Z | |
refterms.versionFCD | AM | |
refterms.dateFOA | 2019-01-23T15:10:20Z | |
refterms.panel | B | en_GB |