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Hot Jupiters are among the best-studied exoplanets, but it is still poorlyunderstood how their chemical composition and cloud properties vary withlongitude. Theoretical models predict that clouds may condense on the nightsideand that molecular abundances can be driven out of equilibrium by zonal winds.Here we report a phase-resolved emission spectrum of the hot Jupiter WASP-43bmeasured from 5-12 $\mu$m with JWST's Mid-Infrared Instrument (MIRI). Thespectra reveal a large day-night temperature contrast (with average brightnesstemperatures of 1524$\pm$35 and 863$\pm$23 Kelvin, respectively) and evidencefor water absorption at all orbital phases. Comparisons with three-dimensionalatmospheric models show that both the phase curve shape and emission spectrastrongly suggest the presence of nightside clouds which become optically thickto thermal emission at pressures greater than ~100 mbar. The dayside isconsistent with a cloudless atmosphere above the mid-infrared photosphere.Contrary to expectations from equilibrium chemistry but consistent withdisequilibrium kinetics models, methane is not detected on the nightside(2$\sigma$ upper limit of 1-6 parts per million, depending on modelassumptions).

Nightside clouds and disequilibrium chemistry on the hot Jupiter WASP-43b