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Lava planets are rocky exoplanets that orbit so close to their host star thattheir day-side is hot enough to melt silicate rock. Their short orbital periodsensure that lava planets are tidally locked into synchronous rotation, withpermanent day and night hemispheres. Such asymmetric magma oceans have noanalogs in the Solar System and will exhibit novel fluid dynamics.  Here we report numerical simulations of lava planet interiors showing thatsolid-liquid fractionation in the planetary interior has a major impact on thecompositional structure and evolution of the planet. We explored two styles ofdynamics that depend primarily on the interior thermal state : 1) a hot fullymolten interior, and 2) a mostly solid interior with a shallow day-side magmaocean.  In the hot interior scenario, the atmosphere reflects the planet's bulksilicate composition and the night-side crust is gravitationally unstable andconstantly replenished. In the cool interior scenario, the distilled atmospherewill lack Na, K and FeO, and the night-side mantle is entirely solid, with acold surface. These two end-member cases can be distinguished with observationsfrom the James Webb Space Telescope, offering an avenue to probe the diversityof terrestrial exoplanet evolutions.

Lava planets interior dynamics govern the long-term evolution of their magma oceans