  Ascertaining rocky exoplanets dynamic evolution requires better understanding
of key internal thermophysical processes that shaped their geological surfaces,
heat fluxes, volatiles and atmospheric content. New high-pressure experiments
on iron and silicates compressible, melting and transport properties are
providing new constraints that demand reassessments of super-Earths thermal and
magnetic evolution models. We examine the interior structure, temperature
distribution, thermal states and dynamo action of these planets with masses
ranging from 1-10 ME. We show that the shallow adiabaticity of iron-alloys and
perovskite or stishovite silicates compared to their liquidus at high pressure
would allow for deep basal magma oceans, and frozen iron cores in planets
larger than 4 ME. The presence and partitioning of MgO may alter this scenario.
For the more massive planets, the dramatic reduction in liquid silicates
viscosity should ensure a vigorous convection in the lower mantle, while the
rise of iron thermal conductivity under high pressures, is shown to keep the
internal cores of planets more massive than 2.5 ME subadiabatic and
non-convicting. This will preclude the dynamo action in the more massive
super-Earths (SE). Our results could allow a new mineral physics centered
classification of terrestrial-like superEarths.
