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Energy balance models (EBMs), alongside radiative-convective climate models(RCMs) and global climate models (GCMs), are useful tools for simulatingplanetary climates. Historically, planetary and exoplanetary EBMs have solelybeen 1D latitudinally-dependent models with no longitudinal dependence, untilthe study of Okuya et al., which focused on simulating synchronously-rotatingplanets. Following the work of Okuya et al., I have designed the first 2D EBM(PlaHab) that can simulate N2-CO2-H2O-H2 atmospheres of both rapidly-rotatingand synchronously-rotating planets, including Mars, Earth, and exoplanetslocated within their circumstellar habitable zones. PlaHab includes physics forboth water and CO2 condensation. Regional topography can be incorporated. Here,I have specifically applied PlaHab to investigate present Earth, early Mars,TRAPPIST-1e and Proxima Centauri b, representing examples of habitable (andpotentially habitable) worlds in our solar system and beyond. I compare my EBMresults against those of other 1D and 3D models, including those of the recentTrappist-1 Habitable Atmosphere (THAI) comparison project. Overall, EBM resultsare consistent with those of other 1D and 3D models although inconsistenciesamong all models continue to be related to the treatment of clouds and otherknown differences between EBMs and GCMs, including heat transportparameterizations. Although two-dimensional EBMs are a relatively new entry inthe study of planetary/exoplanetary climates, their ease-of-use, speed,flexibility, wide applicability, and greater complexity (relative to 1Dmodels), may indicate an ideal combination for the modeling of planetary andexoplanetary atmospheres alike.

A New 2D Energy Balance Model For Simulating the Climates of Rapidly- and Slowly-Rotating Terrestrial Planets