I want people to use my codes (all wonderfully written in FORTRAN) so they are readily available to anyone that wants to use them. If you need help running/setting them up for your particular research application, and/or would like to collaborate on a project of mutual interest using these models, please contact me (rramirez dot elsi.jp) and I’ll be glad to help you get started.
My climate model is capable of simulating the climates of any terrestrial planet with N2, O2, CO2, H2O, CH4, or H2 atmospheres (or any mixture of the above). Ozone, argon, and a wide variety of collision-induced absorption pairs relevant for terrestrial planets at both high and low atmospheric pressures are all included. The code is composed of 55 infrared and 38 solar intervals. This model is extremely versatile as it has been successfully used to simulate Earth (both modern and early), Mars (both present and early), Venus, runaway greenhouses, and a wide range of planets from the inner to outer edge of the habitable zone. If you publish work using this model, a good paper to cite is Ramirez (2017). WARNING: This code does not run on Macs. It must run on some version of Linux either locally or remotely (e.g. ssh).
My latitudinally-dependent energy balance climate model is a rather advanced version of its type, combining the best aspects of mutidimensional (i.e. GCMs) models but it operates at a fraction of the computational cost. The model is non-grey and has 18 ten-degree latitude bands, ice-albedo feedback, ocean heat transport (approximated as diffusion), clouds, and continents. It can be used to model multidimensional effects, including eccentricity, obliquity, and rotation rate. The model has been successfully used to model exoplanets, including ocean worlds, and earlier versions of this model have simulated early Mars. The radiative transfer is parameterized directly from the single-column climate model described above. Indeed, this is effectively a 2-D model when both codes are coupled in this manner. Please cite Ramirez and Levi (2018) for any work that comes out of using this model.
TOTALDISTRIBUTION (correlated-k distribution code)
This code reads in absorption cross-sections from line-by-line radiative transfer models and convert them into absorption (correlated-k) coefficients to be used in climate models. The code is nominally written to read in line-by-line data from KSPECTRUM output files but with a slight rewrite (several lines of code) it can be used to extract data from any line-by-line radiative transfer code. I have used this code to create all of the k-coefficients that are used by my climate models. Ramirez et al. (2014a) and Ramirez et al. (2014b) are good to cite if you publish using this program.