  We present results from an atmospheric circulation study of nine hot Jupiters
that comprise a large transmission spectral survey using the Hubble and Spitzer
Space Telescopes. These observations exhibit a range of spectral behavior over
optical and infrared wavelengths which suggest diverse cloud and haze
properties in their atmospheres. By utilizing the specific system parameters
for each planet, we naturally probe a wide phase space in planet radius,
gravity, orbital period, and equilibrium temperature. First, we show that our
model "grid" recovers trends shown in traditional parametric studies of hot
Jupiters, particularly equatorial superrotation and increased day-night
temperature contrast with increasing equilibrium temperature. We show how
spatial temperature variations, particularly between the dayside and nightside
and west and east terminators, can vary by hundreds of K, which could imply
large variations in Na, K, CO and CH4 abundances in those regions. These
chemical variations can be large enough to be observed in transmission with
high-resolution spectrographs, such as ESPRESSO on VLT, METIS on the E-ELT, or
with MIRI and NIRSpec aboard JWST. We also compare theoretical emission spectra
generated from our models to available Spitzer eclipse depths for each planet,
and find that the outputs from our solar-metallicity, cloud-free models
generally provide a good match to many of the datasets, even without additional
model tuning. Although these models are cloud-free, we can use their results to
understand the chemistry and dynamics that drive cloud formation in their
atmospheres.
