  TRAPPIST-1e is a tidally locked rocky exoplanet orbiting the habitable zone
of an M dwarf star. Upcoming observations are expected to reveal new rocky
exoplanets and their atmospheres around M dwarf stars. To interpret these
future observations we need to model the atmospheres of such exoplanets. We
configured CESM2-WACCM6, a chemistry climate model, for the orbit and stellar
irradiance of TRAPPIST-1e assuming an initial Earth-like atmospheric
composition. Our aim is to characterize the possible ozone (O$_3$) distribution
and explore how this is influenced by the atmospheric circulation shaped by
orography, using the Helmholtz wind decomposition and meridional mass
streamfunction. The model included Earth-like orography and the substellar
point was located over the Pacific Ocean. For such a scenario, our analysis
reveals a North-South asymmetry in the simulated O$_3$ distribution. The O$_3$
concentration is highest below 10 hPa level (below $\sim$30 km) near the South
pole. This asymmetry results from the presence of land masses on the night side
that cause drag in near-surface flows and lead to an asymmetric meridional
overturning circulation. Catalytic species were roughly symmetrically
distributed and were not found to be primary driver for the O$_3$ asymmetry.
The total ozone column (TOC) density was higher for TRAPPIST-1e compared to
Earth, with 8000 Dobson Units (DU) near the South pole and 2000 DU near the
North pole. The results emphasize the sensitivity of O$_3$ to model parameters,
illustrating how incorporating Earth-like orography can affect atmospheric
dynamics and O$_3$ distribution. This link between surface features and
atmospheric dynamics underlines the importance of how changing model parameters
used to study exoplanet atmospheres can influence the interpretation of
observations.
