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14 results for “Magma Ocean”
Data associated with "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs"
<p>The data included here involves all simulations outlined in the manuscript "The Role of Magma Oceans in Maintaining Surface Water on Rocky Planets Orbiting M-Dwarfs", submitted to MNRAS. Files are divided between models with and without a basal magma ocean, as well as different host stars, different magma ocean saturation limits, and different fringe/sensitivity analysis checks. Files are further sub-divided based on our studied parameter space: each is for a single orbital distance within the habitable zone, and a single initial water inventory. "MO_only" files correspond to the concurrent surface magma ocean/runaway greenhouse phase, while "combined_MO_cycling" files correspond to the deep-water cycling period.</p>
The influence of rotation on the preservation of heterogeneities in magma oceans
<p>This dataset contains the data, and codes used to produce the figures, from the upcoming article "The influence of rotation on the preservation of heterogeneities in magma oceans", published in XXX. </p>
Data used in the figures of the article "A cool runaway greenhouse without surface magma ocean"
<p>These data have been generated with the codes Exo k and PCM.</p> <p>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.</p> <p>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</p> <p> </p> <p> </p>
Data for the article "Tidal heating in a subsurface magma ocean on Io revisited"
<p>The data files for the figures in the article "Tidal heating in a subsurface magma ocean on Io revisited". The structure of the files are given in the first row of each file. The file "figure2.dat" only consists of the data for Figure 2a, where Figure 2b andFiguresFigurec are part of Figure 1is.</p>
Data for the article 'Love numbers for Io with a magma ocean'
<p>Data sets for the article 'Love numbers of Io with a magma ocean'. The given file has the following structure and can be used to generate figures 2-5 in the manuscript</p> <p>Depth l (km) log10(visocisty (Pa s)) Ocean thickness (km) Dissipation (TW) k20 k22c k22s Delta_t20 (h) Delta_t22c (h) Delta_t22s (h).</p> <p>In case of any inquiries, please send an email to aygun@karel.troja.mff.cuni.cz.</p>
Supporting dataset for manuscript "Direct viscosity measurement of peridotite melt under lower-mantle conditions supports a fractional magma ocean solidification at top lower mantle conditions"
<p>Supporting material for manuscript "<strong>Direct viscosity measurement of peridotite melt under lower-mantle conditions supports a fractional magma ocean solidification at top lower mantle conditions"</strong></p>
Output files for Degassing of CO2 triggers large-scale loss of helium from magma oceans
<p>This upload includes output files for the paper Degassing of CO2 triggers large-scale loss of helium from magma oceans.</p>
Speciation data for "Genesis of a CO2-rich and H2O-depleted atmosphere from the Earth's early global magma ocean"
<p>Here we present the speciation statistics for volatile-bearing pyrolite melts. For computational details and nomenclature, please refer to the manuscript, "Genesis of a CO2-rich and H2O-depleted atmosphere from the Earth’s early global magma ocean" by N.V. Solomatova and R. Caracas.</p> <p>The data is organized by composition and temperature.</p> <p>File names contain the lattice parameter (e.g., a16.0) in Angstroms, indicating that the cell is 16x16x16 Angstroms in size, for example. The corresponding volumes and densities are tabulated in each folder (e.g., "4CO_4000K_densities.dat"). </p> <p>The first column of each *stat.dat file contains the species type. Long species (e.g., Na_1Ca_2Fe_4Mg_30Al_3Si_24O_93C_4) typically represent the silicate melt and short species (e.g., O_1C_1 and O_2C_1) represent the vapor phase. Underscores represent subscripts (e.g., O_2C_1 denotes a CO2 molecule). The second column is the lifetime of the species in femtoseconds. The third column is the percent of the total. The fourth column is the number of elements in each species (e.g., O_1C_1 has 2 elements and O_2C_1 has 3 elements). Note that the majority of the "H_1" species represent free protons within the melt phase.</p>
Negligible fractionation between fluorine and chlorine during magma ocean crystallization and implications for the origin of Earth's volatiles
<p>Research data underlying all figures in the main text and supplementary material . </p>
Data used for the paper "Birth and decline of magma oceans in planetesimals. Part 2: Structure and thermal history of early accreted small planetary bodies". Submitted to JGR - Planets.
<p>Script and data to generates the figures displayed in the pre-print.</p>
Output files for Degassing of Noble Gases from the Magma Ocean
<p>This upload includes output files for the paper Degassing of noble gases from the magma ocean.</p>
Data sharing of Trace element partitioning between apatite and silicate melts: Effects of major element composition, temperature, and oxygen fugacity, and implications for the volatile element budget of the lunar magma ocean
<p>This repository contains all data used in <strong>Ji and Dygert (2024)</strong>, along with two essential tools (Apatite_Kd_calculator.xlsx):</p> <p>1. A calculator for apatite trace element partition coefficients</p> <p>2. A Eu-in-apatite–plagioclase oxybarometer</p> <p><strong>Update (2025-07-15 version):</strong></p> <p>This version corrects a minor typo in the molecular weight of SiO₂ used in both tools. While the original error had a negligible effect on the calculated partition coefficients, this correction ensures full accuracy for future applications.</p>
Fractional crystallization of a Martian magma ocean and formation of a thermochemical boundary layer at the base of the mantle
Open the record for dataset details and reuse information.
Atmospheric speciation of rocky planets from magma ocean outgassing
<p>EPSC 2020, session TP3, presentation slides + video recording</p>
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