Table 4

Planetary characteristics of the TRAPPIST-1 planets derived from our 1D numerical climate simulations.

Planet Mcore Rcore Rtransit Psurf, H2/CH4 Ptransit, H2/CH4 Psurf, H2/H2O Ptransit, H2/H2O
T1-b 1.02 1.01 1.12 5 0.2 5 0.2
T1-c 1.18 1.06 1.10 1 0.2 1 0.3
T1-d 0.281 0.697 0.766 2 0.3 2 0.3
T1-e 0.766 0.913 0.913 × × × ×
T1-f 0.926 0.986 1.05 5 0.4 cond. cond.
T1-g 1.14 1.05 1.15 2×101 0.4 cond. cond.
T1-h 0.313 0.719 0.775 2 0.4 cond. cond.

Notes. Mcore and Rcore are the mass and radius of the core, with a composition assumed to be Fe/Mg = 0.75 and Mg/Si = 1.02. Rtransit are the transit radii measured by Spitzer. Adopted masses and radii are expressed in Earth units (M and R, respectively). Surface pressures Psurf (i.e. the pressure at the core or atmosphere boundary) and transit pressures Ptransit (i.e. the atmospheric pressure at the transit radius) are expressed in bars. CH4 and H2 O volume mixing ratios were arbitrarily fixed according to C/O solar abundances; that is, 5 × 10−4 and 1 × 10−3, respectively.“cond.” indicates those cases where water vapour (at solar abundance) starts to condense in the atmosphere, and should thus be highly depleted. We note that, given the assumptions made on the core composition, TRAPPIST-1e cannot accommodate a H2 -dominated atmosphere at all.

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