Detailed Evolution grids for TRAPPIST-1 e, f and g with MagmOcV2.0

Here, we show a more detailed 31x11 grid of end states of magma ocean simulations with respect to initial H2O mass and CO2 mass that is scaled with initial \ce{H2O} mass for albedos 0.75 and 0. To generate this finer grid, the corrected gray atmosphere model is used. For the initial H2O mass, 31 values with logarithmic spacing between 1 TO and 100~TO were used. For the initial CO2 mass fractions to be multiplied with initial \ce{H2O} mass, 11 values with linear spacing of 0.1 between 0 and 1 were selected. An initial CO2 mass fraction of 1 indicates that initial CO2 mass is equal to initial \ce{H2O} mass. An initial CO2 mass fraction of zero indicates the absence of \ce{CO2} in the magma ocean.

The detailed grids support the conclusions drawn from the coarser grid, generated with the RT grid atmosphere model. Specifically, for TRAPPIST-1 e, the magma ocean extension with more CO2 is demonstrated around initial water mass of 10 TO, which is clearly associated with a more oxidized mantle for both, albedo 0.75 and 0. 

For TRAPPIST-1 g, a subtle feedback effect on abiotic O2 is noticeable for 6 TO initial H2O mass. The increase in O2 partial pressures by up to 30% coincides with the maximum initial H2O mass, for which significant H2O mass loss can occur. Closer inspection (not shown) reveals that the increase in abiotic O2 build-up occurs, when the atmosphere composition transitions from being \ce{H2O}-dominated to CO2-dominated due to H2O erosion. Since the magma ocean is already solidified at this time, there is no effect on the mantle oxidation.

We note that we stop for these grids the simulation when the planets reach the habitable zone. Simulations with albedo 0 and large initial water mass (>10~TO H2O) enter the habitable zone while still being in the magma ocean stage. Consequently, they show no abiotic atmospheric O2 build-up. About 50-100~bar O2 is, however, already stored in the mantle for all investigated planets with albedo equal zero, indicating significant oxidation of the mantle.

This section is part of the Appendix for the paper: From CO$_2$- to H$_2$O-dominated atmospheres and back