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dc.contributor.authorCarone, Ludmila
dc.contributor.authorBaeyens, Robin
dc.contributor.authorMollière, Paul
dc.contributor.authorBarth, Patrick
dc.contributor.authorVazan, Allona
dc.contributor.authorDecin, Leen
dc.contributor.authorSarkis, Paula
dc.contributor.authorVenot, Olivia
dc.contributor.authorHenning, Thomas
dc.identifier.citationCarone , L , Baeyens , R , Mollière , P , Barth , P , Vazan , A , Decin , L , Sarkis , P , Venot , O & Henning , T 2020 , ' Equatorial anti-rotating day side wind flow in WASP-43b elicited by deep wind jets? ' , Monthly Notices of the Royal Astronomical Society , vol. 496 , no. 3 , pp. 3582–3614 .
dc.identifier.otherPURE: 267585213
dc.identifier.otherPURE UUID: 739fc567-8e90-4362-9f7f-834bb02bea27
dc.identifier.otherORCID: /0000-0002-5418-0882/work/77525198
dc.identifier.otherWOS: 000574919300061
dc.identifier.otherScopus: 85091771226
dc.descriptionFunding: LC acknowledges funding by DLR grant 50OR1804. RB is PhD fellow of the Research Foundation – Flanders (FWO). LD acknowledges support from the ERC consolidator grant 646758 AEROSOL and the FWO Research Project grant G086217N. OV thanks the CNRS/INSU Programme National de Planétologie (PNP) and CNES for funding support. PM acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme under grant agreement 6945713. PS acknowledges the support from the Swiss National Science Foundation under grant BSSGI0155816 ‘PlanetsInTime’. Parts of this work have been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation.en
dc.description.abstractWe present WASP-43b climate simulations with deep wind jets (down to 700 bar) that are linked to retrograde (westward) flow at the equatorial day side for p < 0.1 bar. Retrograde flow inhibits efficient eastward heat transport and naturally explains the small hotspot shift and large day-night-side gradient of WASP-43b (Porb = Prot = 0.8135 d) observed with Spitzer. We find that deep wind jets are mainly associated with very fast rotations (Prot = Porb ≤ 1.5 d) which correspond to the Rhines length smaller than 2 planetary radii. We also diagnose wave activity that likely gives rise to deviations from superrotation. Further, we show that we can achieve full steady state in our climate simulations by imposing a deep forcing regime for p > 10 bar: convergence time-scale τconv = 106–108 s to a common adiabat, as well as linear drag at depth (p ≥ 200 bar), which mimics to first-order magnetic drag. Lower boundary stability and the deep forcing assumptions were also tested with climate simulations for HD 209458b (Porb = Prot = 3.5 d). HD 209458b simulations always show shallow wind jets (never deeper than 100 bar) and unperturbed superrotation. If we impose a fast rotation (Porb = Prot = 0.8135 d), also the HD 209458b-like simulation shows equatorial retrograde flow at the day side. We conclude that the placement of the lower boundary at p = 200 bar is justified for slow rotators like HD 209458b, but we suggest that it has to be placed deeper for fast-rotating, dense hot Jupiters (Porb ≤ 1.5 d) like WASP-43b. Our study highlights that the deep atmosphere may have a strong influence on the observable atmospheric flow in some hot Jupiters.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2020 the Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at
dc.subjectPlanets and satellites: atmospheresen
dc.subjectStars: individual: WASP-43en
dc.subjectBinaries: closeen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSDG 13 - Climate Actionen
dc.titleEquatorial anti-rotating day side wind flow in WASP-43b elicited by deep wind jets?en
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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