Abstract
We will begin by presenting the orbital evolution of the terrestrial planets, which is chaotic but has a low probability of leading to macroscopic instability over the course of the Sun’s lifetime. We will then discuss their physical properties, particularly the size of their metallic cores—which varies greatly from Mercury to the Moon—as well as their chemical properties. We will focus in particular on the degree of oxidation of the various planets and on the deficit of volatile and siderophile elements in the Earth’s mantle. We will also discuss the role of terrestrial planets in the context of the isotopic dichotomy of the Solar System. Finally, we will examine the various scenarios proposed for the origin of water on Earth.
