On the nature of the motion of a test particle in the pseudo-Newtonian Hill system

Zotos, Euaggelos E.; Steklain, Andre Fabiano

doi:10.1007/s10509-019-3668-z

Cited by 5 publications

(2 citation statements)

References 23 publications

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“…Since is a well-known fact that pseudo-Newtonian potentials can have a remarkable effect on the dynamics of different systems (Steklain & Letelier 2006;Dubeibe et al 2017;Zotos & Steklain 2019;, in the present paper we shall use the pseudo-Newtonian Paczyński-Wiita potential (Paczyński & Wiita 1980), for modeling the central part of a galaxy hosting a supermassive black hole, while the flat thin disk is represented by the Miyamoto-Nagai potential. Aiming to obtain direct outcomes on how the mimicked relativistic properties of the supermassive black hole affect the character of the trajectories of the stars, we study the influence of the Schwarzschild radius and the angular momentum of a test particle on the orbit classification, i.e., collisional, ordered, and chaotic.…”

Section: Introductionmentioning

confidence: 99%

Orbit classification in a disk galaxy model with a pseudo-Newtonian central black hole

Zotos

Dubeibe

Steklain

et al. 2020

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We numerically investigate the motion of stars on the meridional plane of an axially symmetric disk galaxy model, containing a central supermassive black hole, represented by the Paczyński-Wiita potential. By using this pseudo-Newtonian potential we can replicate important relativistic properties such as the existence of the Schwarzschild radius. After classifying extensive samples of initial conditions of trajectories, we managed to distinguish between collisional, ordered, and chaotic motion. Besides all starting conditions of regular orbits were further classified into families of regular orbits. Our results are presented via color-coded basin diagrams on several types of two-dimensional planes. Our analysis reveals that both the mass of the black hole (in direct relation with the Schwarzschild radius) as well as angular momentum play an important role in the character of the orbits of stars. More specifically, the trajectories of low angular momentum stars are highly affected by the mass of the black hole, while high angular momentum stars seem to be unaffected by the central black hole. A comparison with previous related outcomes, using Newtonian potentials for the central region of the galaxy, is also made.

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Section: Introductionmentioning

confidence: 99%

Orbit classification in a disk galaxy model with a pseudo-Newtonian central black hole

Zotos

Dubeibe

Steklain

et al. 2020

A&A

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“…Application of the Hill problem with appropriate modifications in the stellar dynamics is discussed in [3]. A pseudo-Newtonian Hill problem was investigated in [4][5][6]. In this model the Newtonian potential is replaced by the Paczyński-Wiita potential [7].…”

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Integrability of the generalised Hill problem

2021

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We consider a certain two-parameter generalisation of the planar Hill lunar problem. We prove that for nonzero values of these parameters the system is not integrable in the Liouville sense. For special choices of parameters the system coincides with the classical Hill system, the integrable synodical Kepler problem or the integrable parametric Hénon system. We prove that the synodical Kepler problem is not super-integrable, and that the parametric Hénon problem is super-integrable for infinitely many values of the parameter.

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On the Stability of the Triangular Equilibrium Points in the Photogravitational R3BP with an Oblate Infinitesimal and Triaxial Primaries for the Binary Lalande 21258 System

Gyegwe

Vincent²,

Perdiou

2022

Approximation and Computation in Science and Engineering

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On the nature of the motion of a test particle in the pseudo-Newtonian Hill system

Cited by 5 publications

References 23 publications

Orbit classification in a disk galaxy model with a pseudo-Newtonian central black hole

Orbit classification in a disk galaxy model with a pseudo-Newtonian central black hole

Integrability of the generalised Hill problem

On the Stability of the Triangular Equilibrium Points in the Photogravitational R3BP with an Oblate Infinitesimal and Triaxial Primaries for the Binary Lalande 21258 System

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