Planet e is the most likely to support a habitable environment, with Earth-like surface temperatures and possibly liquid water oceans. We show that TRAPPIST-1d and e can avoid entering a runaway greenhouse state. 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. Here we compute the heat flux due to insolation and tidal heating for the inner four planets. 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.Īims. Sydney Institute for Astronomy, School of Physics A28, University of Sydney, Sydney, NSW 2006, AustraliaĬontext. Gothard Astrophysical Observatory, ELTE Eötvös Loránd University, Szombathely, Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences,Į-mail: and Geophysical Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Astronomical objects: linking to databases.Including author names using non-Roman alphabets.Suggested resources for more tips on language editing in the sciences Punctuation and style concerns regarding equations, figures, tables, and footnotes
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