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Equilibrium points and their stability in the restricted four-body problem

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TLDR
Numerically the problem of four bodies moving in circles around their center of mass fixed at the origin of the coordinate system, according to the solution of Lagrange where they are always at the vertices of an equilateral triangle, is studied.
Abstract
We study numerically the problem of four bodies, three of which are finite, moving in circles around their center of mass fixed at the origin of the coordinate system, according to the solution of Lagrange where they are always at the vertices of an equilateral triangle, while the fourth is infinitesimal. The fourth body does not affect the motion of the three bodies (primaries). The allowed regions of motion as determined by the zero-velocity surface and corresponding equipotential curves as well as the positions of the equilibrium points are given. The existence and the number of collinear and noncollinear equilibrium points of the problem depend on the mass parameters of the primaries. For three unequal masses, collinear equilibrium solutions do not exist. Critical masses associated with the existence and the number of equilibrium points, are given. The stability of the relative equilibrium solutions in all cases is also studied. The regions of the basins of attraction for the equilibrium points of the present dynamical model for some values of the mass parameters are illustrated.

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Fractal basins of attraction in the planar circular restricted three-body problem with oblateness and radiation pressure

TL;DR: In this paper, the authors used the multivariate version of the Newton-Raphson method to determine the basins of attraction associated with the equilibrium points in a planar circular restricted three-body problem.
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Equilibrium points in the photogravitational restricted four-body problem

TL;DR: In this article, the authors considered the photogravitational version of the problem of four bodies, where an infinitesimal particle is moving under the Newtonian gravitational attraction of three bodies which are finite, moving in circles around their center of mass fixed at the origin of the coordinate system, according to the solution of Lagrange where they are always at the vertices of an equilateral triangle.
Journal ArticleDOI

Families of periodic orbits in the restricted four-body problem

TL;DR: In this article, families of simple symmetric and non-symmetric periodic orbits in the restricted four-body problem are presented, and their linear stability in three cases, i.e., when the three primary bodies are equal, when two primaries are equal and finally when we have three unequal masses.
Journal ArticleDOI

Stability regions of equilibrium points in restricted four-body problem with oblateness effects

TL;DR: In this article, the authors extended the basic model of the restricted four-body problem by introducing two bigger dominant primaries m�� 1 and m petertodd 2 as oblate spheroids when masses of the two primary bodies (m�� 2 and m�� 3) are equal.
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Revealing the basins of convergence in the planar equilateral restricted four-body problem

TL;DR: In this paper, the authors used the planar equilateral restricted four-body problem where two of the primaries have equal masses to determine the Newton-Raphson basins of convergence associated with the equilibrium points.
References
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Theory of Orbits.

TL;DR: In this paper, a book on theory of orbits covering restricted problem of three bodies, two bodies in rotating coordinate system and periodic orbits is presented. But it does not cover the problem of periodic orbits.
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Relative equilibrium solutions in the four body problem

TL;DR: A survey of solutions for arbitrary masses, discussing the manifolds of degeneracy, is given in this paper, where linear stability is analyzed in the restricted and general cases, and values of the masses ensuring linear stability are given.
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The resonant structure of Jupiter's Trojan asteroids – I. Long‐term stability and diffusion

TL;DR: In this paper, the authors studied the global dynamics of the jovian Trojan asteroids by means of the frequency map analysis and classified the main resonant structures that serve as skeleton of the phase space near the Lagrangian points.
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Collinear equilibrium points of Hill’s problem with radiation and oblateness and their fractal basins of attraction

TL;DR: In this paper, the existence, location, and stability of the collinear equilibrium points of a generalized hill problem with radiation of the primary (the Sun) and oblateness of the secondary (the planet) were discussed.
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