  Transmission spectroscopy supports the presence of uncharacterised,
light-scattering and -absorbing aerosols in the atmospheres of many exoplanets.
The complexity of factors influencing the formation, 3-D transport, radiative
impact, and removal of aerosols makes it challenging to match theoretical
models to the existing data. Our study simplifies these factors to focus on the
interaction between planetary general circulation and haze distribution at the
planetary limb. We use an intermediate complexity general circulation model,
ExoPlaSim, to simulate idealised organic haze particles as radiatively active
tracers in the atmospheres of tidally locked terrestrial planets for 32
rotation rates. We find three distinct 3-D spatial haze distributions,
corresponding to three circulation regimes, each with a different haze profile
at the limb. All regimes display significant terminator asymmetry. In our
parameter space, super-Earth-sized planets with rotation periods greater than
13 days have the lowest haze optical depths at the terminator, supporting the
choice of slower rotators as observing targets.
