  Hot Jupiters exhibit large day-night temperature contrasts. Their cooler
nightsides are thought to host clouds. However, the exact nature of these
clouds, their spatial distribution, and their impact on atmospheric dynamics,
thermal structure, and spectra is still unclear. We investigate the atmosphere
of WASP-43 b, a short period hot Jupiter recently observed with JWST, to
understand the radiative and dynamical impact of clouds on the atmospheric
circulation and thermal structure. We aim to understand the impact of different
kinds of condensates potentially forming in WASP-43 b, with various sizes and
atmospheric metallicities. We used a 3D global climate model (GCM) with a new
temperature-dependent cloud model that includes radiative feed-backs coupled
with hydrodynamical integrations to study the atmospheric properties of WASP-43
b. We produced observables from our simulations and compared them to spectral
phase curves from various observations. We show that clouds have a net warming
effect, meaning that the greenhouse effect caused by clouds is stronger than
the albedo cooling effect. We show that the radiative effect of clouds has
various impacts on the dynamical and thermal structure of WASP-43 b. Depending
on the type of condensates and their sizes, the radiative-dynamical feedback
will modify the horizontal and vertical temperature gradient and reduce the
wind speed. For super-solar metallicity atmospheres, fewer clouds form in the
atmosphere, leading to a weaker feedback. Comparisons with spectral phase
curves observed with HST, Spitzer, and JWST indicate that WASP-43 b s nightside
is cloudy and rule out sub-micron Mg2SiO4 cloud particles as the main opacity
source. Distinguishing between cloudy solar and cloudy super-solar-metallicity
atmospheres is not straightforward, and further observations of both reflected
light and thermal emission are needed.
