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 a coupled 3-D atmospheric dynamics and radiative transfer model topredict the disk-integrated thermal emission spectra of transiting exoplanetsin edge-on orbits. We calculate spectra at high resolution to examine theextent to which high-resolution emission spectra are influenced by 3-Datmospheric dynamics and planetary rotation, and to determine whether and howwe can constrain thermal structures and atmospheric dynamics throughhigh-resolution spectroscopy. This study represents the first time that theline-of-sight geometry and resulting Doppler shifts from winds and rotationhave been treated self-consistently in an emission spectrum radiative transfermodel, which allow us to assess the impact of the velocity field on thermalemission spectra. We apply our model to predict emission spectra as a functionof orbital phase for three hot Jupiters, HD 209458b, WASP-43b and HD 189733b.We find net Doppler shifts in modeled spectra due to a combination of winds androtation at a level of 1-3 km/s. These Doppler signatures vary in aquasi-sinusoidal pattern over the course of the planets' orbits as the hotspots approach and recede from the observer's viewpoint. We predict thatWASP-43b produces the largest Doppler shift due to its fast rotation rate. Wefind that the net Doppler shift in an exoplanet's disk-integrated thermalemission spectrum results from a complex combination of winds, rotation, andthermal structure. However, we offer a simple method that estimates themagnitude of equatorial wind speeds in hot Jupiters through measurements of netDoppler shifts and lower resolution thermal phase curves.

Constraining Hot Jupiter Atmospheric Structure and Dynamics through Doppler Shifted Emission Spectra