Application of binary pulsars to axisymmetric bodies in the Elliptic R3BP

Singh, Jagadish; Umar, Aishetu

doi:10.1007/s10509-013-1585-0

Cited by 16 publications

(9 citation statements)

References 59 publications

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“…The asteroids in this case are only influenced by the gravitational forces of the Sun and Jupiter, and the orbit of Jupiter around the Sun is assumed to be a fixed ellipse. The influence of the eccentricity of the orbits of the primary bodies on the existence of the equilibrium points and their stability has been the subject of a number of communications [11]- [26]. The families of symmetric-periodic orbits in the three-dimensional elliptic problem with a variation of the mass ratio μ and the eccentricity e were studied by Sarris (1989).…”

Section: Introductionmentioning

confidence: 99%

The Collinear Libration Points in the Elliptic R3BP with a Triaxial Primary and an Oblate Secondary

Singh¹,

Umar²

2014

IJAA

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This paper examines the motion of a dust grain around a triaxial primary and an oblate companion orbiting each other in elliptic orbits about their common barycenter in the neighborhood of collinear libration points. The positions and stability of these points are found to be affected by the triaxiality and oblateness of the primaries, and by the semi-major axis and eccentricity of their orbits. The stability behavior of the collinear points however remains unchanged; they are unstable in the Lyapunov sense.

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Section: Introductionmentioning

confidence: 99%

The Collinear Libration Points in the Elliptic R3BP with a Triaxial Primary and an Oblate Secondary

Singh¹,

Umar²

2014

IJAA

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“…Equations (11), (14) and (17) are ninth degree equations and some of these equations ((11), (14) and (17)) have more than one positive real root, but in each case there is only one physically acceptable root which corresponds to one of the three collinear libration points (…”

Section: Positions Of the Collinear Libration Pointsmentioning

confidence: 99%

“…He found that an allowance for direct solar radiation pressure results in a change in the positions of the libration points. This has been intensively studied over five decades, by several researchers like [7][8][9][10][11][12][13][14][15], since a large percentage of astronomical bodies are emitters of radiation.…”

Section: Introductionmentioning

confidence: 99%

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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“…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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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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Application of binary pulsars to axisymmetric bodies in the Elliptic R3BP

Cited by 16 publications

References 59 publications

The Collinear Libration Points in the Elliptic R3BP with a Triaxial Primary and an Oblate Secondary

The Collinear Libration Points in the Elliptic R3BP with a Triaxial Primary and an Oblate 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

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

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