Magma ocean evolution of Trappist-1 g


Thermal and volatile evolution of Trappist-1 g’s mantle and atmosphere during its magma ocean phase. This example assumes the initial water inventory is twice modern Earth’s value. Radiogenic and tidal heating of the mantle are included via the modules RadHeat and EqTide, respectively. Atmospheric escape of hydrogen and oxygen is included via the AtmEsc module.




Patrick Barth

Planet name

Trappist-1 g

Initial water content

2 TO


AtmEsc, EqTide, MagmOc, RadHeat, STELLAR

Approx. runtime

1 minute

To run this example


Expected output


Evolution of various planetary parameters for the magma ocean evolution of Trappist-1 g with an initial water inventory of two times modern Earth’s value. Counter-clockwise from top left: Mantle and surface temperature; water masses in the different reservoirs; atmospheric pressures; atmospheric net cooling flux; radiogenic and tidal heating rates; mass fraction of water and Fe2O3 in the melt; oxygen mass in different reservoirs; solidification radius of the magma ocean. The high-frequency variations in the atmospheric flux and oxygen mass in the solid are numerical artifacts due to the fact that the greenhouse effect forces the cooling flux to be low and the surface temperature to stay constant over a long time.