Migration of celestial bodies in the solar system (original) (raw)

Migration of celestial bodies in the solar system and in some exoplanetary systems

Solar System Research, 2024

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. In addition to the theory of coaccretion and the mega-impact and multi-impact models, 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. Along with the Nice model and the “grand tack” model, a model is considered in which the embryos of Uranus and Neptune increased the semimajor axes of their orbits from values of no more than 10 AU to present values only due to gravitational interactions with planetesimals (without the motions of Jupiter and Saturn entering into resonance). 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. It is noted that about 20% of the ejected bodies that left the Earth’s sphere of influence eventually fell back to the Earth. 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.

NUMERICAL STUDY OF THE MIGRATION OF BODIES IN THE FORMATION OF THE SOLAR SYSTEM

International Applied Mechanics, 1992

Our results are consistent with an initial mass of the protoplanetary cloud of MN ~0.04-0.1 Ms ( Ms is the mass of the Sun) assumed by many authors. More icy and stony matter may have entered the core and shell of Jupiter than any other planet. The total mass of bodies penetrating into the asteroid belt from the zones of the giant planets could have been tens of times the mass of the Earth. The system of giant planets expanded during accumulation of these planets. In order for Jupiter and Saturn to have their current eccentricities and their present periods of axial rotation and inclinations of the axes of rotation, nuclei of unformed planets with masses equal to several times the mass of the Earth must have existed in their feed zones. The nuclei of Uranus and Neptune with initial masses equal to several times the mass of the Earth could have migrated from the zone of Saturn, moving along slightly elliptical orbits. The same conclusion can be made for the migration from the zone of Jupiter of the nucleus of Saturn with a mass equal to several dozen times the mass of the Earth. In addition to the nuclei of Uranus and Neptune, other smaller objects could have migrated in the same way from the zones of Jupiter and Saturn into the zones of Uranus and Neptune. The total mass of bodies reaching beyond Neptune's orbit could have reached tens of times the mass of the Earth. Planetesimals could exist at the present time in the zone of Neptune, moving along eccentric and inclined orbits [4]. The average eccentricity of the orbits of bodies migrating into the trans-Neptune belt from the zones of the giant planets is larger than the average eccentricity of bodies formed in the trans-Neptune belt. At the present time bodies could migrate to the Earth's orbit from the asteroid and trans-Neptune belts, and also from the zones of Uranus and Neptune and from the Oort and Hills clouds.

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

Physics – Uspekhi, 2023

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.

The Motion of Celestial Bodies

2011

The history of celestial mechanics is first briefly surveyed, identifying the major contributors and their contributions. The Ptolemaic and Copernican world models, Kepler’s laws of planetary motion and Newton’s laws of universal gravity are presented. It is shown that the orbit of a body moving under the gravitational attraction of another body can be represented by a conic section. The six orbital elements are defined, and it is indicated how they can be determined from observed positions of the body on the sky. Some special cases, permitting exact solutions of the motion of three gravitating bodies, are also treated. With two-body motion as a first approximation, the perturbing effects of other bodies are next derived and applied to the motions of planets, satellites, asteroids and ring particles. The main effects of the Earth’s oblateness on the motions of artificial satellites are explained, and trajectories for sending a space probe from one planet to another are shown. The in...

Formation and migration of trans-Neptunian objects and asteroids

arXiv: Astrophysics, 2002

The evolution of thousands of orbits of Jupiter-family comets and asteroids under the gravitational influence of planets was calculated. Comparison of the results obtained by a symplectic method with those obtained by direct integration showed that a symplectic method is not always good for investigations of the orbital evolution of such bodies. Basing on the results of orbital evolution of bodies, we concluded that a considerable portion of near-Earth objects could have come from the trans-Neptunian region. Some large trans-Neptunian objects could be formed by the compression of rarefied dust condensations, but not by the accumulation of smaller planetesimals.

Migration of bodies to the Earth and the Moon from different distances from the Sun

The Ninth Moscow Solar System Symposium 9M-S3 (Space Research Institute, Moscow, Russia, October 8-12, 2018). https://ms2018.cosmos.ru/ , # 9MS3-SB-11, p. 104-106, 2018

Probabilities of collisions with the Earth and the Moon for bodies with initial eccentricities equaled to 0.3 and inclinations equaled to 0.15 rad were calculated for initial semi-major axes from 2 to 40 AU. The probabilities calculated for 250 bodies can differ by more than a factor of several tens for different runs with similar orbits. The mean probabilities of collisions of bodies with the Earth for the region between 5 and 10 AU exceeded 4×10^-6. On average, for the region between 20 and 35 AU the probabilities could exceed 10^-6. For bodies initially located in the asteroid belt, the probabilities of their col- lisions with the Earth were about 10^-4-10^-3, i.e., were much greater than for bodies initially located beyond Jupiter’s orbit. The ratio of the probabilities of collisions of considered planetesimals with the Earth to those with the Moon was mainly in the range from 16 to 17.

Notes on the Motion of Celestial Bodies

JAMP, 2020

A novel method for the computation of the motion of multi-body systems is proposed against the traditional one, based on the dynamic exchange of attraction forces or using complex field equations, that hardly face two-body problems. The Newton gravitational model is interpreted as the emission of neutrino/gravitons from celestial bodies that combine to yield a cumulative flux that interacts with single bodies through a momentum balance. The neu-trino was first found by Fermi to justify the energy conservation in β decay and, using his model; we found that the emission of neutrino from matter is almost constant independently from the nuclides involved. This flux can be correlated to Gauss constant G, allowing the rebuilding of Newton law on the basis of nuclear data, the neutrino weight and the speed of light. Similarly to nature, we can therefore separate in the calculations the neutrino flux, that represents the gravitational field, is dependent on masses and is not bound to the number of bodies involved, from the motion of each body that, given the field, is independent of the mass of bodies themselves. The conflict between exchanges of forces is avoided, the mathematics is simplified, the computational time is reduced to seconds and the stability of result is guaranteed. The example of computation of the solar system including the Sun and eight planets over a period of one to one hundred years is reported, together with the evolution of the shape of the orbits.

Two mechanisms of natural transport in the Solar System

Communications in Nonlinear Science and Numerical Simulation, 2012

Some minor bodies in the solar system (i.e., comets, asteroids and planetary ejecta) are capable of performing transfers from their original location to very distant places, provided they possess sufficiently large energies. Some of them can reach the surface of a planet. This phenomenon is called natural transport. Within the planar circular restricted three-body problem (PCR3BP) with the Sun and a planet as primaries, and also within two coupled PCR3BPs, the gravity of the secondary causes long-term perturbations and the minor body performs swingbys at the secondary, thus resulting in different behaviours with respect to those observed in the heliocentric two-body model. In this contribution, two natural transport mechanisms in the PCR3BP framework are considered. The first is a short-time transport, consisting in heteroclinic connections between libration point orbits of pairs of Sun-planet PCR3BPs: by varying the relative orbital phase of the involved planets at the start of the transfer, the location of the Poincaré section at which the connection is sought and the size of the departure and arrival periodic orbits, the intersection between the associated unstable and stable manifolds (respectively in the departure and arrival PCR3BP) is computed. The second mechanism corresponds to a long-time transport, the result of the strongly chaotic motion of the minor body in the PCR3BP: the heliocentric orbit changes significantly due to the gravitational interactions with the Sun and the planets (especially the giant planets), and this eventually allows the minor body to reach the vicinity of some planet. In this contribution we provide an analysis of the natural transport in solar system by these two mechanisms. In particular we discuss the key properties of the natural transport, such as the possibility of transferring between two specified celestial bodies, the type of transport and the time of flight. The final aim is to get a deeper insight into the motion of the minor bodies and the exchange of natural material in the solar system.

Application of recent results on the orbital migration of low mass planets: convergence zones

Proceedings of the International Astronomical Union, 2010

Previous models of the combined growth and migration of protoplanets needed large ad hoc reduction factors for the type I migration rate as found in the isothermal approximation. In order to eliminate these factors, a simple semi-analytical model is presented that incorporates recent results on the migration of low mass planets in non-isothermal disks. It allows for outward migration. The model is used to conduct planetary populations synthesis calculations. Two points with zero torque are found in the disks. Planets migrate both in-and outward towards these convergence zones. They could be important for accelerating planetary growth by concentrating matter in one point. We also find that the updated type I migration models allow the formation of both close-in low mass planets, but also of giant planets at large semimajor axes. The problem of too rapid migration is significantly mitigated.