Effect of the Planetesimal Belt on the Dynamics of the Restricted Problem of 2 + 2 Bodies

Mahato, Govind; Pal, Ashok; Alhowaity, Sawsan; Abouelmagd, Elbaz I.; Kushvah, Badam Singh

doi:10.3390/app12010424

Cited by 9 publications

(1 citation statement)

References 23 publications

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“…Mahato et al (2022a) extended the study of classical CRTBP by considering a disk-like structure and an elongated body. Mahato et al (2022b) investigated the stability of equilibrium points within a framework of the perturbed restricted 2 + 2 body problem, taking into account the influence of a disk-like structure.…”

Section: Introductionmentioning

confidence: 99%

Studying the Equilibrium Points of the Modified Circular Restricted Three-body Problem: The Case of Sun–Haumea System

Nurul Huda,

Dermawan,

Saputra

et al. 2023

Res. Astron. Astrophys.

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We intend to study a modified version of the planar Circular Restricted Three-Body Problem (CRTBP) by incorporating several perturbing parameters. We consider the bigger primary as an oblate spheroid and emitting radiation while the small primary has an elongated body. We also consider the perturbation from a disk-like structure encompassing this three-body system. First, we develop a mathematical model of this modified CRTBP. We have found there exist five equilibrium points in this modified CRTBP model, where three of them are collinear and the other two are non-collinear. Second, we apply our modified CRTBP model to the Sun–Haumea system by considering several values of each perturbing parameter. Through our numerical investigation, we have discovered that the incorporation of perturbing parameters has resulted in a shift in the equilibrium point positions of the Sun–Haumea system compared to their positions in the classical CRTBP. The stability of equilibrium points is investigated. We have shown that the collinear equilibrium points are unstable and the stability of non-collinear equilibrium points depends on the mass parameter μ of the system. Unlike the classical case, non-collinear equilibrium points have both a maximum and minimum limit of μ for achieving stability. We remark that the stability range of μ in non-collinear equilibrium points depends on the perturbing parameters. In the context of the Sun–Haumea system, we have found that the non-collinear equilibrium points are stable.

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Section: Introductionmentioning

confidence: 99%