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 Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present the first three-dimensional circulation models for extrasolar gasgiant atmospheres with geometrically and energetically consistent treatments ofmagnetic drag and ohmic dissipation. Atmospheric resistivities are continuouslyupdated and calculated directly from the flow structure, strongly coupling themagnetic effects with the circulation pattern. We model the hot Jupiters HD189733b (Teq \approx 1200 K) and HD 209458b (Teq \approx 1500 K) and testplanetary magnetic field strengths from 0 to 30 G. We find that even at B = 3 Gthe atmospheric structure and circulation of HD 209458b are strongly influencedby magnetic effects, while the cooler HD 189733b remains largely unaffected,even in the case of B = 30 G and super-solar metallicities. Our models of HD209458b indicate that magnetic effects can substantially slow down atmosphericwinds, change circulation and temperature patterns, and alter observableproperties. These models establish that longitudinal and latitudinal hot spotoffsets, day-night flux contrasts, and planetary radius inflation areinterrelated diagnostics of the magnetic induction process occurring in theatmospheres of hot Jupiters and other similarly forced exoplanets. Most of theohmic heating occurs high in the atmosphere and on the day side of the planet,while the heating at depth is strongly dependent on the internal heat fluxassumed for the planet, with more heating when the deep atmosphere is hot. Wecompare the ohmic power at depth in our models, and estimates of the ohmicdissipation in the bulk interior (from general scaling laws), to evolutionarymodels that constrain the amount of heating necessary to explain the inflatedradius of HD 209458b. Our results suggest that deep ohmic heating cansuccessfully inflate the radius of HD 209458b for planetary magnetic fieldstrengths of B \geq 3 - 10 G.

Three-Dimensional Atmospheric Circulation Models of HD 189733b and HD 209458b with Consistent Magnetic Drag and Ohmic Dissipation