Abstract
Abstract
Hot Jupiter atmospheric circulation can be shaped by a range of processes and planetary parameters, including rotation rate, irradiation gradients from tidal synchronization, magnetic effects, gravity, and clouds. Observations of exoplanetary spectral Doppler shifts as a function of phase, made possible with high-resolution spectrographs, can now probe the effects of exoplanetary winds at several points throughout transit. However, these measurements are difficult to interpret, given the variety of relevant atmospheric mechanisms. In this work, we generate high-resolution transmission spectra from two sets of circulation models: self-consistent dynamical models and idealized models that isolate circulation components. We identify how the strength of the jet—or the absence of one—alters the resultant net Doppler shifts. We find that the jet strength most prominently affects Doppler shifts during ingress and egress. During midtransit, the strength of the jet linearly influences the Doppler shifts’ slope; however, this effect is generally secondary to the overall blueshifting from planetary rotation. The slope induced by equatorial jets contrasts with the effect of pure day–night flows, which tend to add constant offsets to Doppler shifts during transit. Our modeling shows that jets also impact the cross correlation function width; faster jets increase velocity dispersion across the limbs. We complement our simulations with semianalytical arguments indicating that first-order changes of the cross correlation function centroid and width (but not amplitude) probe thermal and velocity asymmetries. This work provides recommendations for interpreting net Doppler shifts in transmission and connecting these shifts with exoplanets’ atmospheric circulation.