Migration of celestial bodies in the Solar system and in several exoplanetary systems

Abstract

A review of the results on the migration of celestial bodies in the Solar System and in some exoplanetary systems is presented. Some problems of planet accumulation and migration of planetesimals, small bodies and dust in the forming and present Solar System are considered. It has been noted that the outer layers of the Earth and Venus could have accumulated similar planetesimals from different areas of the feeding zone of the terrestrial planets.The formation of the embryos of the Earth and the Moon from a common rarefied condensation with subsequent growth of the main mass of the embryo of the Moon near the Earth is also discussed. The influence of changes in the semimajor axis of Jupiter's orbit on the formation of the asteroid belt is discussed, as well as the influence of planetesimals from the feeding zone of the giant planets on the formation of bodies beyond the orbit of Neptune. The migration of bodies to the terrestrial planets from different distances from the Sun is considered. It is noted that bodies from the feeding zone of the giant planets and from the outer asteroid belt could deliver to the Earth a quantity of water comparable to the mass of water in the Earth's oceans. The migration of bodies ejected from the Earth is considered. The probabilities of collisions of dust particles with the Earth are usually an order of magnitude greater than the probabilities of collisions of their parent bodies with the Earth. The migration of planetesimals is considered in exoplanetary systems Proxima Centauri and TRAPPIST-1. The amount of water delivered to the inner planet Proxima Centauri b, may have been more than the amount delivered to the Earth. The outer layers of neighboring planets in the TRAPPIST-1 system may contain similar material if there were many planetesimals near their orbits during the late stages of planetary accumulation.

14 pages

References in corpus (29)

• Building Terrestrial Planets
• Towards planetesimals: dense chondrule clumps in the protoplanetary nebula
• Dynamics of the giant planets of the solar system in the gaseous proto-planetary disk and relationship to the current orbital architecture
• Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
• How to form planetesimals from mm-sized chondrules and chondrule aggregates
• Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks
• Multiple Impact Origin for the Moon
• Embryos grown in the dead zone: Assembling the first protoplanetary cores in low mass self-gravitating circumstellar disks of gas and solids
• Formation of pebble-pile planetesimals
• The early instability scenario: terrestrial planet formation during the giant planet instability, and the effect of collisional fragmentation
• Planet formation by pebble accretion in ringed disks
• The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
• The terrestrial planet formation paradox inferred from high-resolution N-body simulations
• Migration processes in the Solar System and their role in the evolution of the Earth and planets
• The early instability scenario: Mars' mass explained by Jupiter's orbit
• A race against the clock: Constraining the timing of cometary bombardment relative to Earth's growth
• Formation of wide-orbit giant planets in protoplanetary disks with a decreasing pebble flux
• Can the giant planets of the Solar System form via pebble accretion in a smooth protoplanetary disc?
• Formation of the Earth and Moon: Influence of Small Bodies
• Formation of trans-Neptunian satellite systems at the stage of condensations
• Origin of orbits of secondaries in the discovered trans-Neptunian binaries
• Number of near-Earth objects and formation of lunar craters over the last billion years
• Depths of Copernican craters on lunar maria and highlands
• Stable Orbits in the Feeding Zone of the Planet Proxima Centauri c
• Delivery of icy planetesimals to inner planets in the Proxima Centauri planetary system
• Origin of the Moon and Lunar Water
• 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