Migration processes in the Solar System and their role in the evolution of the Earth and planets

Abstract

We discuss problems of planetesimal migration in the emerging Solar System and exoplanetary systems. Protoplanetary disk evolution models and the formation of planets are considered. The formation of the Moon and of the asteroid and trans-Neptunian belts is studied. We show that Earth and Venus could acquire more than half of their mass in 5 million years, and their outer layers could accumulate the same material from different parts of the feeding zone of these planets. The migration of small bodies toward the terrestrial planets from various regions of the Solar System is simulated numerically. Based on these computations, we conclude that the mass of water delivered to the Earth by planetesimals, comets, and carbonaceous chondrite asteroids from beyond the ice line could be comparable to the mass of Earth's oceans. The processes of dust migration in the Solar System and sources of the zodiacal cloud are considered.

30 pages, 9 figures

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Cited by in corpus (6)

• Delivery of icy planetesimals to inner planets in the Proxima Centauri planetary system
• Growth of the Moon due to bodies ejected from the Earth
• Motion of Planetesimals in the Hill Sphere of the Star Proxima Centauri
• Probabilities of collisions of bodies ejected from forming Earth with the terrestrial planets
• Migration of celestial bodies in the Solar system and in several exoplanetary systems
• A planet or primordial black hole in the outer region of the Solar system and the dust flow near Earth orbit