  The $24^{\circ}$ N jet borders the North Tropical Belt and North Tropical
Zone, and is the fastest prograde jet on Jupiter, reaching speeds above $170$
m/s. In this region, observations have shown several periodic convective
plumes, likely from latent heat release from water condensation, which affect
the cloud and zonal wind structure of the jet. We model this region with the
Explicit Planetary hybrid-Isentropic Coordinate model using its active
microphysics scheme to study the phenomenology of water and ammonia clouds
within the jet region. On perturbing the atmosphere, we find that an upper
tropospheric wave develops that directly influences the cloud structure within
the jet. This wave travels at $\sim75$ m/s in our model, and leads to periodic
chevron-shaped features in the ammonia cloud deck. These features travel with
the wave speed, and are subsequently much slower than the zonal wind at the
cloud deck. The cloud structure, and the slower drift rate, were both observed
following the convective outbreak in this region in 2016 and 2020. We find that
an upper level circulation is responsible for these cloud features in the
aftermath of the convective outbursts. The comparatively slower observed drift
rates of these features, relative to the wind speed of the jet, provides
constraints on the vertical wind shear above the cloud tops, and we suggest
that wind velocities determined from cloud tracking should correspond to a
different altitude compared to the $680$ hPa pressure level. We also diagnose
the convective potential of the atmosphere due to water condensation, and find
that it is strongly coupled to the wave.
