Motion in the ER3BP with an oblate primary and a triaxial stellar companion

Umar, Aishetu; Hussain, Aminu Abubakar

doi:10.1007/s10509-016-2918-6

Cited by 12 publications

(8 citation statements)

References 51 publications

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“…The equations of motion of a test particle in the ER3BP with a bigger oblate primary and a radiating-triaxial secondary in dimensionless-pulsating (rotating) coordinate system ( , , ) are given in [5,6] as follows:…”

Section: Equations Of Motionmentioning

confidence: 99%

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Generalized Out-of-Plane Equilibrium Points in the Frame of Elliptic Restricted Three-Body Problem: Impact of Oblate Primary and Luminous-Triaxial Secondary

Hussain

Umar

2019

Advances in Astronomy

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This paper studies the motion of a third body near the 1st family of the out-of-plane equilibrium points, L6,7, in the elliptic restricted problem of three bodies under an oblate primary and a radiating-triaxial secondary. It is seen that the pair of points (ξ0,0,±ζ0) which correspond to the positions of the 1st family of the out-of-plane equilibrium points, L6,7, are affected by the oblateness of the primary, radiation pressure and triaxiality of the secondary, semimajor axis, and eccentricity of the orbits of the principal bodies. But the point ±ζ0 is unaffected by the semimajor axis and eccentricity of the orbits of the principal bodies. The effects of the parameters involved in this problem are shown on the topologies of the zero-velocity curves for the binary systems PSR 1903+0327 and DP-Leonis. An investigation of the stability of the out-of-plane equilibrium points, L6,7 numerically, shows that they can be stable for 0.32≤μ≤0.5 and for very low eccentricity. L6,7 of PSR 1903+0327 and DP-Leonis are however linearly unstable.

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Section: Equations Of Motionmentioning

confidence: 99%

“…Over decades, the study of the existence of some families of particular solutions in both circular and elliptic R3BP has received the attention of various researchers like [1][2][3][4][5][6][7][8][9][10][11][12][13] among others.…”

Section: Introductionmentioning

confidence: 99%

Generalized Out-of-Plane Equilibrium Points in the Frame of Elliptic Restricted Three-Body Problem: Impact of Oblate Primary and Luminous-Triaxial Secondary

Hussain

Umar

2019

Advances in Astronomy

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“…The equations of motion of a test particle in the ER3BP with a bigger oblate primary and a triaxial as well as radiating secondary in dimensionless-pulsating coordinate system (ξ ,η , ) ζ are given in [24] as:…”

Section: Equations Of Motionmentioning

confidence: 99%

“…The classical R3BP considers the shape of the finite bodies as purely spherical, but it has been proved that astronomical bodies are not purely spherical [16,17,18,19,20,21,22,23,24]. They are either oblate spheroid or triaxial rigid bodies.…”

Section: Introductionmentioning

confidence: 99%

“…Our aim in this work is to investigate the effects of oblateness of the primary body and the luminosity and triaxiality of the secondary body on the locations as well as linear stability of the collinear libration points. This study is applied in the neighborhood of two binaries CEN X-4 and PSR 1903+0327 barrowed from Umar and Hussain [24].…”

Section: Introductionmentioning

confidence: 99%

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Investigation of the Stability of a Test Particle in the Vicinity of Collinear Points with the Additional Influence of an Oblate Primary and a Triaxial-Stellar Companion in the Frame of ER3BP

Hussain

Umar

Singh

2018

IFSL

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We investigate in the elliptic framework of the restricted three-body problem, the motion around the collinear points of an infinitesimal particle in the vicinity of an oblate primary and a triaxial stellar companion. The locations of the collinear points are affected by the eccentricity of the orbits, oblateness of the primary body and the triaxiality and luminosity of the secondary. A numerical analysis of the effects of the parameters on the positions of collinear points of CEN X-4 and PSR J1903+0327 reveals a general shift away from the smaller primary with increase in eccentricity and triaxiality factors and a shift towards the smaller primary with increase in the semi-major axis and oblateness of the primary on L1. The collinear points remain unstable in spite of the introduction of these parameters.

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Dynamics of a small planetoid in Newtonian gravity field of Lagrangian configuration of three primaries

2023

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Motion in the ER3BP with an oblate primary and a triaxial stellar companion

Cited by 12 publications

References 51 publications

Generalized Out-of-Plane Equilibrium Points in the Frame of Elliptic Restricted Three-Body Problem: Impact of Oblate Primary and Luminous-Triaxial Secondary

Generalized Out-of-Plane Equilibrium Points in the Frame of Elliptic Restricted Three-Body Problem: Impact of Oblate Primary and Luminous-Triaxial Secondary

Investigation of the Stability of a Test Particle in the Vicinity of Collinear Points with the Additional Influence of an Oblate Primary and a Triaxial-Stellar Companion in the Frame of ER3BP

Dynamics of a small planetoid in Newtonian gravity field of Lagrangian configuration of three primaries

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