AGNI: A radiative-convective model for lava planet atmospheres

Abstract

It is important that we are able to accurately model the atmospheres of (exo)planets. This is because atmospheres play a central role in setting a planet's thermochemical environment at a given point in time, and also in regulating how it evolves over geological timescales. Additionally, it is primarily by observation of their atmospheres that we are able to characterise exoplanets. There is particular demand for accurate models in the context of so-called lava worlds: planets with molten interiors (or `magma oceans'). AGNI is a Julia program designed to solve for the temperature and radiation environment within the atmospheres of rocky (exo)planets. It leverages a well established FORTRAN code to calculate radiative fluxes from a given atmospheric temperature structure and composition, which -- alongside representations of convection and other processes -- enables an energy-conserving numerical solution for the atmospheric conditions. In contrast to most other numerical atmosphere models, AGNI uses a Newton-Raphson optimisation method to obtain its solution, which enables improved performance and scalability. Our model was specifically developed for use alongside planetary interior models within a coupled simulation framework. However, it can also be applied to scientific problems standalone when used as an executable program; it reads TOML configuration files and outputs figures and NetCDF datasets. AGNI can also function as a software library; it is used in this sense within the Jupyter notebook tutorials of our GitHub repository (https://nichollsh.github.io/AGNI/dev/)

Published in JOSS

References in corpus (20)

• Ranges of Atmospheric Mass and Composition of Super Earth Exoplanets
• Predictions of the atmospheric composition of GJ 1132b
• Treatment of overlapping gaseous absorption with the correlated-k method in hot Jupiter and brown dwarf atmosphere models
• A secondary atmosphere on the rocky exoplanet 55 Cancri e
• Vertically resolved magma ocean-protoatmosphere evolution: H${}_2$, H${}_2$O, CO${}_2$, CH${}_4$, CO, O${}_2$, and N${}_2$ as primary absorbers
• Was Venus Ever Habitable? Constraints from a Coupled Interior-Atmosphere-Redox Evolution Model
• The erosion of large primary atmospheres typically leaves behind substantial secondary atmospheres on temperate rocky planets
• A cool runaway greenhouse without surface magma ocean
• Super-Earths and Earth-like Exoplanets
• Magma ocean evolution at arbitrary redox state
• Observability of silicates in volatile atmospheres of super-Earths and sub-Neptunes
• A mineralogical reason why all exoplanets cannot be equally oxidising
• Volatile atmospheres of lava worlds
• Redox evolution of the crystallizing terrestrial magma ocean and its influence on atmosphere outgassing
• Convective shutdown in the atmospheres of lava worlds
• Thermal and orbital evolution of low-mass exoplanets
• Self-limited tidal heating and prolonged magma oceans in the L 98-59 system
• Characterising the Atmosphere of 55 Cancri e: 1D Forward Model Grid for Current and Future JWST Observations
• LavAtmos 2.0: Incorporating Volatiles Species in Vaporization Models
• Impact of oxygen fugacity on atmospheric structure and emission spectra of ultra hot rocky exoplanets

Cited by in corpus (2)

• Self-limited tidal heating and prolonged magma oceans in the L 98-59 system
• Volatile-rich evolution of molten super-Earth L 98-59 d