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dc.contributor.authorDrummond, B
dc.contributor.authorMayne, NJ
dc.contributor.authorManners, J
dc.contributor.authorCarter, A
dc.contributor.authorBoutle, I
dc.contributor.authorBaraffe, I
dc.contributor.authorHebrard, E
dc.contributor.authorTremblin, P
dc.contributor.authorSing, D
dc.contributor.authorAmundsen, D
dc.contributor.authorAcreman, D
dc.date.accessioned2018-02-27T11:27:09Z
dc.date.accessioned2018-03-07T09:41:28Z
dc.date.issued2018-03-15
dc.description.abstractWe present a study of the effect of wind-driven advection on the chemical composition of hot Jupiter atmospheres using a fully-consistent 3D hydrodynamics, chemistry and radiative transfer code, the Met Office Unified Model (UM). Chemical modelling of exoplanet atmospheres has primarily been restricted to 1D models that cannot account for 3D dynamical processes. In this work we couple a chemical relaxation scheme to the UM to account for the chemical interconversion of methane and carbon monoxide. This is done consistently with the radiative transfer meaning that departures from chemical equilibrium are included in the heating rates (and emission) and hence complete the feedback between the dynamics, thermal structure and chemical composition. In this letter we simulate the well studied atmosphere of HD 209458b. We find that the combined effect of horizontal and vertical advection leads to an increase in the methane abundance by several orders of magnitude; directly opposite to the trend found in previous works. Our results demonstrate the need to include 3D effects when considering the chemistry of hot Jupiter atmospheres. We calculate transmission and emission spectra, as well as the emission phase curve, from our simulations. We conclude that gas-phase non-equilibrium chemistry is unlikely to explain the model–observation discrepancy in the 4.5 µm Spitzer/IRAC channel. However, we highlight other spectral regions, observable with the James Webb Space Telescope, where signatures of wind-driven chemistry are more prominent.en_GB
dc.description.sponsorshipBD and DKS acknowledge funding from the European Research Council (ERC) under the European Unions Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement no. 336792. NJM is part funded by a Leverhulme Trust Research Project Grant. JM and IAB acknowledge the support of a Met Office Academic Partnership secondment. ALC is funded by an STFC studentship. DSA acknowledges support from the NASA Astrobiology Program through the Nexus for Exoplanet System Science. This work used the DiRAC Complexity system, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility. This equipment is funded by BIS National E-Infrastructure capital grant ST/K000373/1 and STFC DiRAC Operations grant ST/K0003259/1. DiRAC is part of the National E-Infrastructure.en_GB
dc.identifier.citationVol. 855 (2), article L31en_GB
dc.identifier.doi10.3847/2041-8213/aab209
dc.identifier.urihttp://hdl.handle.net/10871/31897
dc.language.isoenen_GB
dc.publisherAmerican Astronomical Society / IOP Publishingen_GB
dc.relation.urlhttp://hdl.handle.net/10871/32579
dc.rights© 2018. The American Astronomical Society. All rights reserved.
dc.titleObservable signatures of wind-driven chemistry with a fully consistent three dimensional radiative hydrodynamics model of HD 209458b (article)en_GB
dc.typeArticleen_GB
dc.identifier.issn2041-8205
dc.descriptionThis is the final version of the article. 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: http://hdl.handle.net/10871/32579
dc.identifier.journalAstrophysical Journal Lettersen_GB


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