ORCID
0000-0001-7553-8444
Keywords
Planetary atmospheres; Solar system terrestrial planets; Earth (planet); Mars; Extrasolar rocky planets; Habitable planets; Planetary climates; Exoplanet atmospheres; TRAPPIST-1e, THAI, Proxima Centauri b
Data Files Description
This 2D energy balance climate model, named PlaHab, is the first such model to simulate N2-CO2-H2O-H2 atmospheres of both rapidly and slowly rotating terrestrial planets in our solar system and beyond (exoplanets). I have recently used it to model Earth, Mars, and tidally-locked exoplanets, including TRAPPIST-1e and Proxima Centauri b (Ramirez 2024). Most results are consistent with those of 3D GCMs. However, PlaHab has the additional advantage of speed. Thus, it combines some of the detail and complexity of 3D models with the speed and ease-of-use of simpler ones, facilitating the exploration of much larger parameter space. This makes it very efficient to quickly check model results against large suites of observational data.
Description of Terms or Variables
README is included.
Abstract
Energy balance models (EBMs), alongside radiative–convective climate models and global climate models (GCMs), are useful tools for simulating planetary climates. Historically, planetary and exoplanetary EBMs have nearly all been 1D latitudinally dependent models with no longitudinal dependence. PlaHab is the first EBM that can simulate N2–CO2–H2O–H2 atmospheres of both rapidly and synchronously rotating planets, including Mars, Earth, and exoplanets located within their circumstellar habitable zones. PlaHab includes physics for both water and CO2 condensation. Regional topography can be incorporated. Overall, EBM results are consistent with those of other 1D and 3D models, although minor differences among all models continue to be related to the treatment of clouds and other known differences between EBMs and GCMs, including heat transport parameterizations. Although 2D EBMs are a relatively new entry in the study of planetary/exoplanetary climates, their ease of use, speed, flexibility, wide applicability, and greater complexity (relative to 1D models) may indicate an ideal combination for the modeling of planetary and exoplanetary atmospheres alike.
Collection Notes
This is a 2D energy balance climate model I developed for the simulation of terrestrial planetary and exoplanetary atmospheres.
Date Collected
2023-10-24
Date Created
2024-01-16
Release Date
1-16-2024
Document Type
Other
Dataset Type
Programming Software Code
Identifier
2D Planetary and Exoplanetary Energy Balance Climate Model
Language
English
Rights
This work is licensed under a Creative Commons Attribution 4.0 International License.
College
science
Campus Location
John C. Hitt Library
Department
Physics
Unit
Planetary Sciences Group
STARS Citation
Ramirez, R.M., 2024, A New 2D Energy Balance Model for Simulating the Climates of Rapidly and Slowly Rotating Terrestrial Planets. Planetary Science Journal, 5, 2 doi:10.3847/PSJ/ad0729
Recommended Citation
Ramirez, R.M., 2024, A New 2D Energy Balance Model for Simulating the Climates of Rapidly and Slowly Rotating Terrestrial Planets. Planetary Science Journal, 5, 2 doi:10.3847/PSJ/ad0729