  Recently acquired Hubble and Spitzer phase curves of the short-period hot
Jupiter WASP-43b make it an ideal target for confronting theory with data. On
the observational front, we re-analyze the 3.6 and 4.5 $\mu$m Spitzer phase
curves and demonstrate that our improved analysis better removes residual red
noise due to intra-pixel sensitivity, which leads to greater fluxes emanating
from the nightside of WASP-43b, thus reducing the tension between theory and
data. On the theoretical front, we construct cloudfree and cloudy atmospheres
of WASP-43b using our Global Circulation Model (GCM), THOR, which solves the
non-hydrostatic Euler equations (compared to GCMs that typically solve the
hydrostatic primitive equations). The cloudfree atmosphere produces a
reasonable fit to the dayside emission spectrum. The multi-phase emission
spectra constrain the cloud deck to be confined to the nightside and have a
finite cloud-top pressure. The multi-wavelength phase curves are naturally
consistent with our cloudy atmospheres, except for the 4.5 $\mu$m phase curve,
which requires the presence of enhanced carbon dioxide in the atmosphere of
WASP-43b. Multi-phase emission spectra at higher spectral resolution, as may be
obtained using the James Webb Space Telescope, and a reflected-light phase
curve at visible wavelengths would further constrain the properties of clouds
in WASP-43b.
