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Here it is shown how to find the interior structure of a variety ofrock-and-iron planetary bodies by using the rock density and some aspects ofthe core density as known for the Earth and using a convection principle forthe iron-rich core. Convection minimizes both the density and temperaturegradients inside the core fluid. This is achieved if the density of the corefluid is close to pure iron melting density at the core-mantle boundary, andthe density has the smallest value possible for iron-rich melt at the innercore boundary. The critical iron densities for both pure iron and iron withmaximal light impurities were previously obtained utilizing Landau's theory offirst order phase transitions with the most reliable experimental scaling. Theplanetary interior density is found by iteratively calculating the gravity andpressure in small radial steps. Moment of inertia factors are also calculatedand agree well for the bodies for which we have accurate measurements: Moon,Mars and Mercury. Calculations are also made for the exoplanets Kepler-78b,K2-229b and Kepler-10b. All show iron-rich liquid in their cores. The lighter,solar objects are without an inner core, but the heaviest two exoplanets have apure iron innermost core inside the inner core. The parameter range for agrowing inner core in the radius-mass plane is calculated. The magnetic fieldfollowing the growth of an inner core protects life on Earth, and similarly forexoplanets. This guides the selection of exoplanets to study in the search forlife.

Interior structure of Mars and other rock-and-iron planetary bodies