Astronomy and Astrophysics, volume 624A, 2-2 (2019/4-1)
Tidal heating and the habitability of the TRAPPIST-1 exoplanets.
DOBOS V., BARR A.C. and KISS L.L.
Abstract (from CDS):
Context. New estimates of the masses and radii of the seven planets orbiting the ultracool M-dwarf TRAPPIST-1 star permit improved modelling of their compositions, heating by tidal dissipation, and removal of tidal heat by solid-state convection.
Aims. Here we compute the heat flux due to insolation and tidal heating for the inner four planets.
Methods. We apply a Maxwell viscoelastic rheology to compute the tidal response of the planets using the volume-weighted average of the viscosities and rigidities of the metal, rock, high-pressure ice, and liquid water/ice I layers.
Results. We show that TRAPPIST-1d and e can avoid entering a runaway greenhouse state. Planet e is the most likely to support a habitable environment, with Earth-like surface temperatures and possibly liquid water oceans. Planet d also avoids a runaway greenhouse, if its surface reflectance is at least as high as that of the Earth. Planets b and c, closer to the star, have heat fluxes high enough to trigger a runaway greenhouse and to support volcanism on the surfaces of their rock layers, rendering them too warm for life. Planets f, g, and h are too far from the star to experience significant tidal heating, and likely have solid ice surfaces with possible subsurface liquid water oceans.
© ESO 2019
planets and satellites: interiors - planets and satellites: terrestrial planets - methods: numerical - astrobiology
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