From dd522d7f6be4cfa465dc66cff56372694f0ab173 Mon Sep 17 00:00:00 2001 From: Harrison Nicholls Date: Sat, 14 Sep 2024 16:54:43 +0100 Subject: [PATCH] Codes links and socrates doi --- docs/paper/paper.bib | 11 +++++++++++ docs/paper/paper.md | 2 +- 2 files changed, 12 insertions(+), 1 deletion(-) diff --git a/docs/paper/paper.bib b/docs/paper/paper.bib index 4b177dc0..2632fc69 100644 --- a/docs/paper/paper.bib +++ b/docs/paper/paper.bib @@ -349,6 +349,17 @@ @article{boukrouche_beyond_2021 pages = {130}, } +@misc{nicholls_socrates_2024, + author = {Nicholls, Harrison}, + title = {SOCRATES and other tools}, + month = jun, + year = 2024, + publisher = {Zenodo}, + version = {v24.03.01}, + doi = {10.5281/zenodo.12190852}, + url = {https://doi.org/10.5281/zenodo.12190852} +} + @book{stamnes_radiative_2017, title = {Radiative {Transfer} in the {Atmosphere} and {Ocean}}, diff --git a/docs/paper/paper.md b/docs/paper/paper.md index 110ebb27..df73c075 100644 --- a/docs/paper/paper.md +++ b/docs/paper/paper.md @@ -37,7 +37,7 @@ Several theoretical studies have modelled the atmospheres and evolution of these Ensuring sufficient spectral resolution is important in modelling the blanketing effect of these atmospheres, as resolving the opacity (and transparency) of their many gases is known to be key in setting the rate at which these planets can cool by radiation to space [@pierrehumbert_book_2010; @boukrouche_beyond_2021]. It is also important that we are able to run grids of models which explore the range of possible (and as-yet poorly constrained) conditions that these planets could exhibit, which demands efficient modelling given finite computational resources. Performance is paramount. -HELIOS[^4] [@malik_helios_2017] is a hydrostatic atmosphere model written in Python and CUDA. HELIOS assumes that the "interior temperature" $T_{\text{int}}$ of a model planet is a known quantity, but coupled time-evolved evolution with an interior model requires that this quantity be an output variable, instead requiring a fixed surface temperature (or something equivalent). It is therefore not possible to apply HELIOS to this problem. The same also applies to Exo_k[5^] [@selsis_cool_2023]. +HELIOS[^4] [@malik_helios_2017] is a hydrostatic atmosphere model written in Python and CUDA. HELIOS assumes that the "interior temperature" $T_{\text{int}}$ of a model planet is a known quantity, but coupled time-evolved evolution with an interior model requires that this quantity be an output variable, instead requiring a fixed surface temperature (or something equivalent). It is therefore not possible to apply HELIOS to this problem. The same also applies to Exo_k[^5] [@selsis_cool_2023]. [^4]: HELIOS can be found on GitHub [here](https://github.com/exoclime/HELIOS). [^5]: Exo_k can be found online [here](https://forge.oasu.u-bordeaux.fr/jleconte/exo_k-public).