This repository provides mass radius data for a range of compositions. The mass radius data is calculated using the interior structure model used in the BICEPS (Bayesian Interior Characterisation of ExoPlanetS) code (Haldemann et al. 2023). The data files can be found in the data directory.
A list of all provided compositions is given in the table below. The header variables are:
- Label: label of the compositon
- wCore: weight fraction of the central core layer
- wRock: weight fraction of the rocky mantle
- wH2O: weight fraction of the pure water layer
- wH/He: weight fraction of the H/He envelope
- xFe,Core: Core composition, molar fraction of Fe
- xS,Core: Core composition, molar fraction of S
- xMgO,Mantle: Mantle composition, molar fraction of MgO
- xSiO2,Mantle: Mantle composition, molar fraction of SiO2
- xFeO,Mantle: Mantle composition, molar fraction of FeO
| Label | wCore | wRock | wH2O | wH/He | xFe,Core | xS,Core | xMgO,Mantle | xSiO2,Mantle | xFeO,Mantle |
|---|---|---|---|---|---|---|---|---|---|
| C0 | 1 | 0 | 0 | 0 | 1 | 0 | N/A | N/A | N/A |
| C1 | 1 | 0 | 0 | 0 | 0.87 | 0.13 | N/A | N/A | N/A |
| R0 | 0 | 1 | 0 | 0 | N/A | N/A | 1 | 0 | 0 |
| R1 | 0 | 1 | 0 | 0 | N/A | N/A | 0.5 | 0.5 | 0 |
| R2 | 0 | 1 | 0 | 0 | N/A | N/A | 0.519 | 0.423 | 0.058 |
| E0 | 0.32 | 0.68 | 0 | 0 | 0.87 | 0.13 | 0.519 | 0.423 | 0.058 |
| W0 | 0 | 0 | 1 | 0 | N/A | N/A | N/A | N/A | N/A |
| W1 | 0.3168 | 0.6732 | 0.01 | 0 | 1 | 0 | 0.5 | 0.5 | 0 |
| W2 | 0.304 | 0.646 | 0.05 | 0 | 1 | 0 | 0.5 | 0.5 | 0 |
| W3 | 0.288 | 0.612 | 0.1 | 0 | 1 | 0 | 0.5 | 0.5 | 0 |
| W4 | 0.16 | 0.34 | 0.5 | 0 | 1 | 0 | 0.5 | 0.5 | 0 |
| D0 | 0.319968 | 0.679932 | 0 | 0.0001 | 1 | 0 | 0.5 | 0.5 | 0 |
| D1 | 0.31968 | 0.67932 | 0 | 0.001 | 1 | 0 | 0.5 | 0.5 | 0 |
| D2 | 0.3168 | 0.6732 | 0 | 0.01 | 1 | 0 | 0.5 | 0.5 | 0 |
| D3 | 0.288 | 0.612 | 0 | 0.1 | 1 | 0 | 0.5 | 0.5 | 0 |
| D4 | 0.256 | 0.544 | 0 | 0.2 | 1 | 0 | 0.5 | 0.5 | 0 |
| N0 | 0.316768 | 0.673132 | 0.01 | 0.0001 | 1 | 0 | 0.5 | 0.5 | 0 |
| N1 | 0.31648 | 0.67252 | 0.01 | 0.001 | 1 | 0 | 0.5 | 0.5 | 0 |
| N2 | 0.3136 | 0.6664 | 0.01 | 0.01 | 1 | 0 | 0.5 | 0.5 | 0 |
| N3 | 0.2848 | 0.6052 | 0.01 | 0.1 | 1 | 0 | 0.5 | 0.5 | 0 |
| N4 | 0.2528 | 0.5372 | 0.01 | 0.2 | 1 | 0 | 0.5 | 0.5 | 0 |
| N5 | 0.287968 | 0.611932 | 0.1 | 0.0001 | 1 | 0 | 0.5 | 0.5 | 0 |
| N6 | 0.28768 | 0.61132 | 0.1 | 0.001 | 1 | 0 | 0.5 | 0.5 | 0 |
| N7 | 0.2848 | 0.6052 | 0.1 | 0.01 | 1 | 0 | 0.5 | 0.5 | 0 |
| N8 | 0.256 | 0.544 | 0.1 | 0.1 | 1 | 0 | 0.5 | 0.5 | 0 |
| N9 | 0.224 | 0.476 | 0.1 | 0.2 | 1 | 0 | 0.5 | 0.5 | 0 |
The data are provided for each composition in a simple csv files. The mass radius data is provided for masses between 0.1 Earth masses and 30 Earth masses. For each mass and composition the transit radius was calculated for five equillibrium temperatures (50 K, 300 K, 800 K,1500 K, 2000 K). The pressure at which the integration of the internal structure was started was always set to 1 barye. Note: it is possible that for some combinations no transit radius is provided. This is the case if the radius of the planet is so big that the outermost layers would not be bound to the planet, for example,in the case of very small masses, high equilibrium temperatures and volatile rich compositions.
If this data is used in a publication do cite the following publication:
- Haldemann, J. and Dorn, C and Venturini, J. and Alibert, Y. and Benz, W., 2023, Astronomy & Astrophysics