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Astrophysical observations reveal a large diversity of radii and masses ofexoplanets. It is important to characterize the interiors of exoplanets tounderstand planetary diversity and further determine how unique, or not, Earthis. Assessing interior structure is challenging because there are few data andlarge uncertainties. Thus, for a given exoplanet a range of interior structuremodels can satisfy available data. Typically, interior models aim to constrainthe radial structure and composition of the core and mantle, and additionallyice, ocean, and gas layer if appropriate. Constraining the parameters of theselayers may also inform us about interior dynamics. However, it remainschallenging to constrain interior dynamics using interior structure modelsbecause structure models are relatively insensitive to the thermal state of aplanet. Nevertheless, elucidating interior dynamics remains a key goal inexoplanetology due to its role in determining surface conditions and hencehabitability. Thus far, Earth-like habitability can be excluded forsuper-Earths that are in close proximity to their stars and therefore have highsurface temperatures that promote local magma oceans.

Assessing the Interior Structure of Terrestrial Exoplanets with Implications for Habitability