DOI: 10.5281/zenodo.6877000
title: Data used in the figures of the article "A cool runaway greenhouse without surface magma ocean"

description: These data have been generated with the codes Exo k and PCM. Exo k is an open-source software. A complete documentation on how to install and use it can be found at http://perso.astrophy.u-bordeaux.fr/∼jleconte/ exo k-doc/index.html.<br> The generic Global Climate Model PCM (formerly known as LMDZ.generic) used in this work is the version 2528 that can be downloaded with documentation from the SVN repository at https://svn.lmd.jussieu.fr/Planeto/trunk/ LMDZ.GENERIC/. More information and documentation are available at http://www-planets.lmd.jussieu.fr. The archive is organized as follows:<br> ├─ Fig1 (comparison of atmospheric profiles with a same Outgoing Thermal Radiation)<br> │ ├─ OTR274.txt (profiles with a 274 W/m2 bolometric emission)<br> │ ├─ OTR10000txt (profiles with a 1000 W/m2 bolometric emission)<br> │<br> ├─ Fig2 (Outgoing Thermal Radiation as a function of surface temperature)<br> │ ├─ Geoflux=0 (internal heat flux = 0 W/m2)<br> │ │ ├─ T1_0_ISR_Tsurf_OTR_ALB.dat<br> │ │ ├─ Proxima_0_ISR_Tsurf_OTR_ALB.dat<br> │ │ ├─ M3_0_ISR_Tsurf_OTR_ALB.dat<br> │ │ ├─ Sun_0_ISR_Tsurf_OTR_ALB.dat<br> │ │ ├─ F1_0_ISR_Tsurf_OTR_ALB.dat<br> │ ├─ Geoflux=0.09Wm-2 (internal heat flux = 0.09 W/m2)<br> │ ├─ T1_0.09_ISR_Tsurf_OTR_ALB.dat<br> │ ├─ Sun_0.09_ISR_Tsurf_OTR_ALB.dat<br> │<br> ├─ Fig3 (Trappist-1b profiles and spectra)<br> │ ├─ Profiles<br> │ │ ├─ Adiabatic<br> │ │ │ ├─ Trappist1b_adiabatic_profile_1EO.txt (1x Earth Ocean)<br> │ │ │ ├─ Trappist1b_adiabatic_profile_3EO.txt (3x Earth Ocean)<br> │ │ │<br> │ │ ├─ Converged<br> │ │ │ ├─ Trappist1b_profile_1EO_geoflux=0W.txt (1x Earth Ocean, internal heat flux = 0 W/m2)<br> │ │ │ ├─ Trappist1b_profile_1EO_geoflux=5W.txt (1x Earth Ocean, internal heat flux = 5 W/m2)<br> │ │ │ ├─ Trappist1b_profile_3EO_geoflux=0W.txt (3x Earth Ocean, internal heat flux = 0 W/m2)<br> │ │ │ ├─ Trappist1b_profile_3EO_geoflux=5W.txt (3x Earth Ocean, internal heat flux = 5 W/m2)<br> │ │ │<br> │ ├─ Spectra<br> │ │ ├─ Adiabatic<br> │ │ │ ├─ Trappist1b_adiabatic_spectra_1EO.txt (1x Earth Ocean)<br> │ │ │ ├─ Trappist1b_adiabatic_spectra_3EO.txt (3x Earth Ocean)<br> │ │ │<br> │ │ ├─ Converged<br> │ │ │ ├─ Trappist1b_spectra_1EO_geoflux=0W.txt (1x Earth Ocean, internal heat flux = 0 W/m2)<br> │ │ │ ├─ Trappist1b_spectra_1EO_geoflux=5W.txt (1x Earth Ocean, internal heat flux = 5 W/m2)<br> │ │ │ ├─ Trappist1b_spectra_3EO_geoflux=0W.txt (3x Earth Ocean, internal heat flux = 0 W/m2)<br> │ │ │ ├─ Trappist1b_spectra_3EO_geoflux=5W.txt (3x Earth Ocean, internal heat flux = 5 W/m2)<br> │<br> ├─ Fig4_(net stellar and emission fluxes for a converged and adiabatic profiles)<br> │ ├─profiles_Sun_adia_converged_netfluxes.txt<br> │<br> ├─ Fig5 (Profiles for different instellations, for each star)<br> │ ├─ T1_profiles.txt<br> │ ├─ Proxima_profiles.txt<br> │ ├─ M3_profiles.txt<br> │ ├─ K5_profiles.txt<br> │ ├─ Sun_profiles.txt<br> │ ├─ F1_profiles.txt<br> │<br> ├─ Fig6 (Comparison 1D vs 3D)<br> │ ├─ 1D<br> │ │ ├─ exok_1D_PTH_trappist1.txt<br> │ │ ├─ exok_1D_PTH_Proxima.txt<br> │ │ ├─ exok_1D_PTH_M3.txt<br> │ ├─ 3D<br> │ ├─ PT_trappist1_3D.dat<br> │ ├─ PT_Proxima_3D.dat<br> │ ├─ PT_M3_3D.dat<br> │ ├─ HeatingRates_3D_trappist1.dat<br> │ ├─ HeatingRates_3D_trappist1.dat<br> │ ├─ HeatingRates_3D_trappist1.dat<br> │<br> ├─ Fig7 (Profiles for 2 values of instellation and 3 values of cp)<br> │ ├─ profiles_cp_Sun.txt <br> │<br> ├─ Fig8 (Profiles for 3 values of instellation and continuums from 2 version of MT_sCKD)<br> │ ├─ profiles_2continuums_Sun.txt <br> │<br> ├─ Fig9 (Profiles as a function of surface pressure and internal heat fluxes)<br> │ ├─ EarlyVenus<br> │ │ ├─ profiles_fig9_EarlyVenus_0.1bar.txt<br> │ │ ├─ profiles_fig9_EarlyVenus_1bar.txt<br> │ │ ├─ profiles_fig9_EarlyVenus_10bar.txt<br> │ │ ├─ profiles_fig9_EarlyVenus_100bar.txt<br> │ │ ├─ profiles_fig9_EarlyVenus_270bar.txt<br> │ ├─ Trappist1<br> │ ├─ profiles_fig9_Trappist1_0.1bar.txt<br> │ ├─ profiles_fig9_Trappist1_1bar.txt<br> │ ├─ profiles_fig9_Trappist1_10bar.txt<br> │ ├─ profiles_fig9_Trappist1_100bar.txt<br> │ ├─ profiles_fig9_Trappist1_270bar.txt<br> │<br> ├─ readme.txt
description: JL and FS acknowledge funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (grant agreement No. 679030/WHIPLASH), and from the french state: CNES, Programme National de Planétologie (PNP), the ANR (ANR-20-CE49-0009: SOUND), and in the framework of the Investments for the Future programme IdEx, Université de Bordeaux/RRI ORIGINS. FS and MT acknowledge support from BELSPO BRAIN (project B2/212/PI/PORTAL). MT acknowledges support from the Tremplin 2022 program of the Faculty of Science and Engineering of Sorbonne University. The authors thank the Generic PCM team for the teamwork development and improvement of the model. MT acknowledges the use of the High-Performance Computing (HPC) resources of Centre Informatique National de l'Enseignement Superieur (CINES) under the allocation A0080110391 made by Grand Equipement National de Calcul Intensif (GENCI), which was essential to compute the 3-D GCM simulations presented in this work. EB and GC acknowledge support from the Swiss National Science Foundation grant 200021 197176. Their work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grants 51NF40 182901 and 51NF40 205606. This research has made use of NASA's Astrophysics Data System.