Abstract
We present medium-wave ($\sim$0.5~$\mu$m to $\sim$13~$\mu$m) radiative flux
distributions and spectra derived from high-resolution atmospheric dynamics
simulations of an exoplanet \WASPP. This planet serves to illustrate several
important features. Assuming different chemical compositions for its atmosphere
(e.g., H$_2$/He only and $Z \in \{1, 12\}$ times solar metallicity), the
outgoing radiative flux is computed using full radiative transfer that folds in
the James Webb Space Telescope (JWST) and Ariel instrument characteristics. We
find that the observed variability depends strongly on the the assumed
chemistry and the instrument wavelength range, hence the probed altitude of the
atmosphere. With H$_2$/He only, the flux and variability originate near the
10$^5$~Pa level; with solar and higher metallicity, $\sim$10$^3$~Pa level is
probed, and the variability is distinguishably reduced. Our calculations show
that JWST and Ariel have the sensitivity to capture the atmospheric variability
of exoplanets like \WASPP, depending on the metallicity -- both in repeated
eclipse and phase-curve observations.