Modeling the interiors of rocky exoplanets in the habitable zone

We have modeled the possible interior structures of habitable zone rocky exoplanets based on their masses and radii. In our model, the planetary interior is divided into four layers: iron core, rocky mantle, high pressure ice and water / ice. In order to assess the habitability of these planets, we have estimated the minimum and maximum H2O content of each exoplanet. We have calculated the tidal heating of the host star as well as the heat flux from the decay of radioactive elements in the interior of the planets. We have estimated whether these processes, along with the incident stellar flux, could provide sufficient energy to melt the upper ice layers and act as a continuous source of heat to sustain liquid water either inside the planet or on the planetary surface. Taking into account all these effects, we have a better understanding of the habitability of these planets. We propose to make new observations of those planets that we have found habitable to better constrain their parameters and to characterize their atmospheres.