Elspeth K. H. Lee's Website

Researching the climates of exoplanet atmospheres

I study the climate of exoplanet and brown dwarf atmospheres, in particular researching the dynamics, temperature structures, chemistry and clouds that affect the observable properties of these atmospheres, focusing on the 3D aspects of planetary atmospheres. For this I use state of the art atmospheric hydrodynamical models, so called, general circulation models (GCMs). I am a lead developer of the Exo-FMS GCM model, as well as having experience with the THOR and MITgcm GCM models. I add specialized physical processes to these models such as radiative-transfer of various flavors (e.g. grey, non-grey and correlated-k), cloud formation physics and kinetic chemistry modeling.

I also develop true 3D radiative-transfer techniques for highly accurate modeling of radiation through a global atmosphere. I am the lead developer of the gCMCRT model, a Monte Carlo RT model that uses GPU technology to accelerate computational times. This can be used to calculate albedo, emission and transmission spectra, as well as perform phase curve calculations. This model can also be used at high resolution, computing the Doppler and rotational shifting of lines, allowing theoretical models to be used to physically interpret high-resolution observational data in detail.

My 1D two-stream RT suites and the 3D gCMCRT model are available on my GitHub.

My Research

(In a nutshell)

  • Exoplanet atmospheric dynamics
  • Atmospheric radiative-transfer
  • 3D GCM modelling
  • Cloud particle formation
  • 3D radiative-transfer with MCRT
  • Kinetic & equilibrium chemistry
  • Gas and cloud opacities
  • HPC & GPU computing solutions

Research Highlights

Coupling dynamic chemistry to GCMs

In Tsai et al. (2022) and Lee et al. (2023) we developed a miniature chemical kinetics scheme `mini-chem' which is highly suitable for coupling to GCM models of exoplanet atmospheres. We found that the chemical species follow the dynamical patterns present in the atmosphere and are significantly out of chemical equilibrium.

Coupling microphysical cloud models to GCMs

In Lee et al. (2016) we coupled the microphysical cloud formation model DIHRT, with the 3D HD 189733b RHD model of Dobbs-Dixon. We found that the clouds undergo a day-night evaporation and condensation cycle, with different species condensing and evaporation across the globe of the exoplanet atmosphere. The cloud structure properties also varied greatly as function of latitude, longitude and depth.

Developing 3D radiative-transfer techniques with MCRT

In Lee et al. (2022) we upgraded the CMCRT model to use GPU technology, decreasing it's runtime by 2-100x. This model is a true 3D RT model, able to accurately produce transmission, emission, albedo spectra and phase curves from GCM output. We also include the ability to perform high-resolution RT modelling, with Doppler and rotational shifting of spectral lines, allowing cross-correlation techniques to be performed with the gCMCRT output. We also developed an opacity package (optools) that can easily interpolate and mix gas phase species opacities as well as CIA, Rayleigh and cloud particle opacities. This code is publically available on GitHub.

Examining two-stream radiative-transfer techniques for hot Jupiter GCMs using Exo-FMS

In Lee et al. (2020) we investigated three different RT techniques for HJ GCM models using the Exo-FMS GCM model, semi-grey, non-grey picket fence and spectral correlated-k. We found that the picket fence scheme was able to reproduce well the correlated-k model, providing a more realistic and intermediate RT solution between the well used semi-grey and correlated-k approaches. This flexible method allows more accurate GCMs to be run in the future without extreme added computational expense. The two stream methods and opacity packages are available on my GitHub

Understanding brown dwarf atmospheres highly irradiated by white dwarf parent stars

In Lee et al. (2022) we investigated the properties of three brown dwarf atmospheres that orbit close to their host stars. For this we also used the Exo-FMS GCM model, developing a multi-band opacity scheme as well as using a correlated-k scheme. We found these atmospheres were dominated by the strong UV absorption in the upper atmosphere, giving rise to large low pressure temperature inversions.