Abstract:<p>This paper studies effects of the triaxiality and radiation pressure of both the primaries on the stability of the infinitesimal motion about triangular equilibrium points in the elliptical restricted three body problem(ER3BP), assuming that the bigger and the smaller primaries are triaxial and the source of radiation as well. It is observed that the motion around these points is stable under certain condition with respect to the radiation pressure and oblate triaxiality. The critical mass ratio depen… Show more
“…In the absence of P-R drags, with oblate luminous primaries, describing circular orbit, our result agrees with [18]; without PR-drags of the primaries, our result coincide with [14,21]. In the presence of PR drag with a bigger luminous primary and a triaxial companion, our result coincide with the findings of [26] while in the case of a smaller oblate body together with a luminous triaxial body, it agrees with [25].…”
Section: Discussionsupporting
confidence: 83%
“…This circular restricted three-body problem (CR3BP) describes the motion of the infinitesimal mass moving in circular orbits and thus will not sufficiently describe the motion when certain perturbing forces are involved. This led scientists and mathematicians into an extensive study of the circular restricted three-body problem (CR3BP) from which models have been developed on the basis of different perturbing forces [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21].…”
Section: Introductionmentioning
confidence: 99%
“…The Authors of [8] described a model with the bigger primary as an oblate spheroid for which the triangular point L 4 is stable for all values of the mass ratio while in [14], the two primaries are treated as rigid triaxial bodies where it was established that the collinear points are unstable as oppose to the triangular points that are stable for a range of mass ratio less than the critical mass ratio. In [18], the problem is examined on the basis that both primaries are oblate spheroids for which the triangular points are stable within a given region while [21] examined the case for which both bodies are triaxial rigid bodies.…”
Abstract. This paper explores the motion of an infinitesimal body around the triangular equilibrium points in the framework of circular restricted three-body problem (CR3BP) with the postulation that the primaries are triaxial rigid bodies, radiating in nature and are also under the influence of Poynting-Robertson (P-R) drag. We study the linear stability of these triangular points and for the numerical application, the binary stars Kruger 60 (AB) and Archird have been considered. These triangular points are not only perceived to move towards the line joining the primaries in the direction of the bigger primary with increasing triaxiality, they are also unstable owing to the destabilizing influence of P-R drag.
“…In the absence of P-R drags, with oblate luminous primaries, describing circular orbit, our result agrees with [18]; without PR-drags of the primaries, our result coincide with [14,21]. In the presence of PR drag with a bigger luminous primary and a triaxial companion, our result coincide with the findings of [26] while in the case of a smaller oblate body together with a luminous triaxial body, it agrees with [25].…”
Section: Discussionsupporting
confidence: 83%
“…This circular restricted three-body problem (CR3BP) describes the motion of the infinitesimal mass moving in circular orbits and thus will not sufficiently describe the motion when certain perturbing forces are involved. This led scientists and mathematicians into an extensive study of the circular restricted three-body problem (CR3BP) from which models have been developed on the basis of different perturbing forces [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21].…”
Section: Introductionmentioning
confidence: 99%
“…The Authors of [8] described a model with the bigger primary as an oblate spheroid for which the triangular point L 4 is stable for all values of the mass ratio while in [14], the two primaries are treated as rigid triaxial bodies where it was established that the collinear points are unstable as oppose to the triangular points that are stable for a range of mass ratio less than the critical mass ratio. In [18], the problem is examined on the basis that both primaries are oblate spheroids for which the triangular points are stable within a given region while [21] examined the case for which both bodies are triaxial rigid bodies.…”
Abstract. This paper explores the motion of an infinitesimal body around the triangular equilibrium points in the framework of circular restricted three-body problem (CR3BP) with the postulation that the primaries are triaxial rigid bodies, radiating in nature and are also under the influence of Poynting-Robertson (P-R) drag. We study the linear stability of these triangular points and for the numerical application, the binary stars Kruger 60 (AB) and Archird have been considered. These triangular points are not only perceived to move towards the line joining the primaries in the direction of the bigger primary with increasing triaxiality, they are also unstable owing to the destabilizing influence of P-R drag.
“…[17]. The differential equation of motion of the third body P in nondimensional barycentre, pulsating and non-uniformly rotating coordinate system (x, y) is written in the form: Where m 1 and m 2 are masses of the primaries.…”
Section: Variational Equation Of Motionmentioning
confidence: 99%
“…[12], Narayan, A., Kumar, C.R. [13], Narayan, A., Singh, N. [14], Narayan, A., Usha, T. [15] , Singh, J., Aishetu, U. (2012), Singh, J., Aishetu, U.…”
This Paper deals with the effects of the radiation pressure and triaxiality of primaries on the stability of infinitesimal motion about triangular equilibrium points [ 4 , 5 ] in the elliptical restricted three body problem (ER3EB) around binary system. For determining the characteristic exponents of variational equations with periodic coefficient, we have used analytical method, described by Bennet in [3,4]. This analytical method is based on Floquet's theory. The stability of equilibrium points has been discussed under the assumption thatboth the primaries are radiating and triaxial. For this we have drawn transition cureves in μ-e plane. And it is seen that system is stable outside the transition curves, while system is Unstable within the transition curves.
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