  Rocky planets hosted by close-in extrasolar systems are likely to be tidally
locked in 1:1 spin-orbit resonance, a configuration where they exhibit
permanent dayside and nightside. Because of the resulting day-night temperature
gradient, the climate and large-scale circulation of these planets are strongly
determined by their atmospheric stability against collapse, which designates
the runaway condensation of greenhouse gases. To better constrain the surface
conditions of rocky planets located in the habitable zone of their host star,
it is therefore crucial to elucidate the mechanisms that govern the day-night
heat redistribution. As a first attempt to bridge the gap between multiple
modelling approaches ranging from idealised models to 3-D General Circulation
Models (GCM), we developed a General Circulation Meta-Model (GCMM) able to
reproduce both the closed-form solutions provided by analytical models and the
numerical solutions obtained from GCM simulations. We used this approach to
characterise the atmospheric stability of Earth-sized rocky planets with dry
atmospheres containing CO2, and we benchmarked it against 3-D GCM simulations
using THOR GCM. We observe that the collapse pressure below which collapse
occurs can vary by ~40% around the value predicted by analytical scaling laws
depending on the mechanisms taken into account among radiative transfer,
atmospheric dynamics, and turbulent diffusion. Particularly, we find (i) that
the turbulent diffusion taking place in the dayside planetary boundary layer
(PBL) globally tends to warm up the nightside surface hemisphere except in the
transition zone between optically thin and optically thick regimes, (ii) that
the PBL also significantly affects the day-night advection timescale, and (iii)
that the slow rotator approximation holds from the moment that the normalised
equatorial Rossby deformation radius is greater than 2.
