English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Simulations with a 3D general circulation model (GCM) suggest that onepotential driver behind the observed radius inflation in hot Jupiters may bethe downward advection of energy from the highly irradiated photosphere intothe deeper layers. Here, we compare dynamical heat transport within thenon-inflated hot Jupiter WASP-43b and the canonical inflated hot Jupiter HD209458b, with similar effective temperatures. We investigate to what extent theradiatively driven heating and cooling in the photosphere (at pressures smallerthan 1 bar) influence the deeper temperature profile (at pressures between 1 to700 bar). Our simulations with the new non-gray 3D radiation-hydrodynamicalmodel expeRT/MITgcm show that the deep temperature profile of WASP-43b isassociated with a relatively cold adiabat. The deep layers of HD 209458b,however, do not converge and remain nearly unchanged regardless of whether acold or a hot initial state is used. Furthermore, we show that different flowstructures in the deep atmospheric layers arise. There, we find that WASP-43bexhibits a deep equatorial jet, driven by the relatively fast tidally lockedrotation of this planet (0.81 days), as compared to HD 209458b (3.47 days).However, by comparing simulations with different rotation periods, we find thatthe resulting flow structures only marginally influence the temperatureevolution in the deep atmosphere, which is almost completely dominated byradiative heating and cooling. Furthermore, we find that the evolution ofdeeper layers can influence the 3D temperature structure in the photosphere ofWASP-43b. Thus, dayside emission spectra of WASP-43b may shed more light ontothe dynamical processes occurring at greater depths.

Exploring the deep atmospheres of HD 209458b and WASP-43b using a non-gray general circulation model