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In this study we investigated the interiors of rocky exoplanets in order toidentify those that may have large quantities of water. We modelled theinteriors of 28 rocky exoplanets, assuming four different layers - an ironcore, a rock mantle, a high-pressure ice layer, and a surface ice/water layer.Due to observational bias, our study is limited to habitable zone exoplanets.We determined a range of possible water mass fractions for each planetconsistent with the modelled planetary structures. We calculated the tidalheating experienced by these exoplanets through gravitational interactions withtheir host stars, assuming a temperature- and composition dependent Maxwellviscoelastic rheology. Assuming radioactive elemental abundances observed inSolar System meteorites, we also calculated the radiogenic heat flux inside theplanets. We estimated the probability of the presence of a thick ocean layer inthese planets, taking into account the effect of both tidal and radiogenicheating. Our results showed that Proxima Centauri b, Ross 128 b, Teegarden's band c, GJ 1061 c and d, and TRAPPIST-1 e may have an extended liquid waterreservoir. Furthermore, extremely high H2O-content of the exoplanets Kepler-62f, Kepler-1652 b, Kepler-452 b, and Kepler-442 b suggests that these planetsmay maintain a water vapour atmosphere and may in fact be examples of largerocean worlds. Upon the discovery of new rocky exoplanets beyond the habitablezone, our study can be extended to icy worlds.

Water content of rocky exoplanets in the habitable zone