Aguda Ekele Vincent
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
Aguda Ekele Vincent has a total of 17 co-authors. Here are the top co-authors by number of shared publications:
- Jagadish Singh
Department of Mathematics, Faculty of Physical Sciences, Ahmadu Bello University, Zaria 810107, Nigeria
5 shared publications - Vassilis Kalantonis
Department of Electrical & Computer Engineering, University of Patras, GR-26504 Patras, Greece
3 shared publications - Angela E. Perdiou
Department of Civil Engineering, University of Patras, GR-26504 Patras, Greece
2 shared publications - George Tsirogiannis
Department of Food Science and Technology, University of Patras, 26504 Patras, Greece
2 shared publications - Joel John Taura
Federal University of Kashere, Gombe State
2 shared publications Amos S. Idowu
Department of Mathematics, University of Ilorin, Nigeria
1 shared publication
Latest Publications
- 1 July 2026
- Published by Pleiades Publishing Ltd in Astronomy Reports
- Vol. 70 (7) , 850-866
On the Existence and Stability of Out-of-Plane Libration Points in the Modified CR3BP with Three-Body Interactions
In the present work, we investigate the motion of an infinitesimal third body near the out-of-plane libration points of the modified circular restricted three-body problem (CR3BP), taking into account the effects of three-body interaction and non-sphericity of the two primary bodies (primaries), under the assumption that the primaries have equal masses and equal oblateness or prolateness. In particular, we examine numerically the number, positions, and linear stability of the out-of-plane libration points under the influence of the perturbing parameters, i.e., three-body interactions parameter \(\left( k \right)\) and non-sphericity coefficient \(\left( A \right)\). It is observed that the number of the out-of-plane libration points of the problem depends on the perturbing parameters. The system is found to allow up to six out-of-plane libration points: two on the Oz axis (\(L_{1}^{z},L_{2}^{z}\)) and four on the Oxz plane outside the Oz and Ox axes \(\left( {L_{{3(4)}}^{{xz}},L_{{5(6)}}^{{xz}}} \right)\). The positions of all libration points shift under variations in the perturbing parameters. Moreover, the non-sphericity parameter is found to exert greater influence on the motion of an infinitesimal body near the out-of-plane libration points than the three-body interactions. Stability analysis shows that the four libration points on the Oxz plane are generally unstable while the two libration points on the Oz axis can exhibit stability for specific combinations of \(\mu ,\;k,\) and \(A\).- 1 July 2026
- Published by Pleiades Publishing Ltd in Astronomy Reports
- Vol. 70 (7) , 850-866
On the Existence and Stability of Out-of-Plane Libration Points in the Modified CR3BP with Three-Body Interactions
In the present work, we investigate the motion of an infinitesimal third body near the out-of-plane libration points of the modified circular restricted three-body problem (CR3BP), taking into account the effects of three-body interaction and non-sphericity of the two primary bodies (primaries), under the assumption that the primaries have equal masses and equal oblateness or prolateness. In particular, we examine numerically the number, positions, and linear stability of the out-of-plane libration points under the influence of the perturbing parameters, i.e., three-body interactions parameter \(\left( k \right)\) and non-sphericity coefficient \(\left( A \right)\). It is observed that the number of the out-of-plane libration points of the problem depends on the perturbing parameters. The system is found to allow up to six out-of-plane libration points: two on the Oz axis (\(L_{1}^{z},L_{2}^{z}\)) and four on the Oxz plane outside the Oz and Ox axes \(\left( {L_{{3(4)}}^{{xz}},L_{{5(6)}}^{{xz}}} \right)\). The positions of all libration points shift under variations in the perturbing parameters. Moreover, the non-sphericity parameter is found to exert greater influence on the motion of an infinitesimal body near the out-of-plane libration points than the three-body interactions. Stability analysis shows that the four libration points on the Oxz plane are generally unstable while the two libration points on the Oz axis can exhibit stability for specific combinations of \(\mu ,\;k,\) and \(A\).- 6 February 2026
- Published by Elsevier in New Astronomy
- Vol. 125
Out-of-plane equilibrium points in the rotating mass dipole model with non-spherical radiating bodies
- 6 February 2026
- Published by Elsevier in New Astronomy
- Vol. 125
Out-of-plane equilibrium points in the rotating mass dipole model with non-spherical radiating bodies
- Open Access
- 3 October 2025
- Published by MDPI AG in Mathematics
- Vol. 13 (19) , 3179
Equilibrium Dynamics in the CR3BP with Radiating Primary and Oblate Secondary Using the Rotating Mass Dipole Model
In this study, we numerically investigate the equilibrium dynamics of a rotating system consisting of two masses connected by a massless rod within the framework of the circular restricted three-body problem. The larger primary is modeled as a radiating body and the smaller as an oblate spheroid. We explore the influence of the involved parameters, i.e., mass ratio (), force ratio (k), radiation pressure factor (), and oblateness coefficient (), on the number, positions, and linear stability of equilibrium points. Zero velocity curves are presented in the equatorial plane for varying values of the Jacobi constant. Up to five equilibrium points are identified of which three are collinear (, , ) and two are non-collinear (, ). The positions of all equilibria shift under variations in the perturbing parameters. While the collinear points are generally unstable, can exhibit stability for certain combinations of , k, and . The non-collinear points may also be stable under specific conditions with stability zones expanding with increased parameter values. The model is applied to the irregular, elongated asteroid 951 Gaspra, for which five equilibrium points are found. Despite positional dependence on oblateness and radiation, the perturbations do not significantly affect the equilibrium points’ stability and the motion near them remains linearly unstable. The Lyapunov families of periodic orbits emanating from the collinear equilibria of this particular system are also investigated.- 3 October 2025
- Published by MDPI AG in Mathematics
- Vol. 13 (19) , 3179
Open AccessEquilibrium Dynamics in the CR3BP with Radiating Primary and Oblate Secondary Using the Rotating Mass Dipole Model
In this study, we numerically investigate the equilibrium dynamics of a rotating system consisting of two masses connected by a massless rod within the framework of the circular restricted three-body problem. The larger primary is modeled as a radiating body and the smaller as an oblate spheroid. We explore the influence of the involved parameters, i.e., mass ratio (), force ratio (k), radiation pressure factor (), and oblateness coefficient (), on the number, positions, and linear stability of equilibrium points. Zero velocity curves are presented in the equatorial plane for varying values of the Jacobi constant. Up to five equilibrium points are identified of which three are collinear (, , ) and two are non-collinear (, ). The positions of all equilibria shift under variations in the perturbing parameters. While the collinear points are generally unstable, can exhibit stability for certain combinations of , k, and . The non-collinear points may also be stable under specific conditions with stability zones expanding with increased parameter values. The model is applied to the irregular, elongated asteroid 951 Gaspra, for which five equilibrium points are found. Despite positional dependence on oblateness and radiation, the perturbations do not significantly affect the equilibrium points’ stability and the motion near them remains linearly unstable. The Lyapunov families of periodic orbits emanating from the collinear equilibria of this particular system are also investigated. - Open Access
- 14 May 2025
- Published by Springer Nature in Discover Space
- Vol. 129 (1) , 1-19
Existence and stability of equilibrium points in the perturbed R3BP with Stokes drag in the binary $\eta -$ Cassiopeiae system- 14 May 2025
- Published by Springer Nature in Discover Space
- Vol. 129 (1) , 1-19
Open AccessExistence and stability of equilibrium points in the perturbed R3BP with Stokes drag in the binary $\eta -$ Cassiopeiae system - Open Access
- 31 March 2025
- Published by MDPI AG in Mathematics
- Vol. 13 (7) , 1150
Equilibrium Points and Periodic Orbits in the Circular Restricted Synchronous Three-Body Problem with Radiation and Mass Dipole Effects: Application to Asteroid 2001SN263
This study numerically explores the dynamics of the photogravitational circular restricted three-body problem, where an infinitesimal particle moves under the gravitational influence of two primary bodies connected by a massless rod. These primary masses revolve in circular orbits around their common center of mass, which remains fixed at the origin of the coordinate system. The distance between the two masses remains constant, independent of their rotation period. The third body, being infinitesimally small compared to the primary masses, has a negligible effect on their motion. The primary mass is considered as a radiating body, while the secondary is modeled as an elongated one comprising two hypothetical point masses separated by a fixed distance. The analysis focuses on determining the number, location, and stability of equilibrium points, as well as examining the structure of zero-velocity curves under the influence of system parameters such as mass and force ratio, radiation pressure and geometric configuration of the secondary body. The system is found to allow up to six equilibria: four collinear and two non-collinear. Their number and positions are significantly affected by variations in the system’s parameters. Stability analysis reveals that the two non-collinear equilibrium points can exhibit stability under specific parameter configurations, while the four collinear points are typically unstable. An exception is the innermost collinear equilibrium point, which can be stable for certain parameter values. Our numerical investigation on periodic orbits around the collinear equilibrium points of the asteroid triple-system 2001SN263 show that a variation, either to the values of radiation or the force ratio parameters, influence their special characteristics such as period and stability. Also, their continuation in the space of initial conditions shows that all families terminate naturally at collision orbits with either the primary or the secondary.
- 31 March 2025
- Published by MDPI AG in Mathematics
- Vol. 13 (7) , 1150
Open AccessEquilibrium Points and Periodic Orbits in the Circular Restricted Synchronous Three-Body Problem with Radiation and Mass Dipole Effects: Application to Asteroid 2001SN263
This study numerically explores the dynamics of the photogravitational circular restricted three-body problem, where an infinitesimal particle moves under the gravitational influence of two primary bodies connected by a massless rod. These primary masses revolve in circular orbits around their common center of mass, which remains fixed at the origin of the coordinate system. The distance between the two masses remains constant, independent of their rotation period. The third body, being infinitesimally small compared to the primary masses, has a negligible effect on their motion. The primary mass is considered as a radiating body, while the secondary is modeled as an elongated one comprising two hypothetical point masses separated by a fixed distance. The analysis focuses on determining the number, location, and stability of equilibrium points, as well as examining the structure of zero-velocity curves under the influence of system parameters such as mass and force ratio, radiation pressure and geometric configuration of the secondary body. The system is found to allow up to six equilibria: four collinear and two non-collinear. Their number and positions are significantly affected by variations in the system’s parameters. Stability analysis reveals that the two non-collinear equilibrium points can exhibit stability under specific parameter configurations, while the four collinear points are typically unstable. An exception is the innermost collinear equilibrium point, which can be stable for certain parameter values. Our numerical investigation on periodic orbits around the collinear equilibrium points of the asteroid triple-system 2001SN263 show that a variation, either to the values of radiation or the force ratio parameters, influence their special characteristics such as period and stability. Also, their continuation in the space of initial conditions shows that all families terminate naturally at collision orbits with either the primary or the secondary.
- 11 February 2025
- Published by Springer Nature in Archive of Applied Mechanics
- Vol. 95 (2) , 1-16
Continuation fraction perturbation effect on out-of-plane equilibrium points
- 11 February 2025
- Published by Springer Nature in Archive of Applied Mechanics
- Vol. 95 (2) , 1-16
Continuation fraction perturbation effect on out-of-plane equilibrium points
- Open Access
Out-of-Plane Equilibrium Points in the Photogravitational Hill Three-Body Problem
This paper investigates the movement of a negligible mass body (third body) in the vicinity of the out-of-plane equilibrium points of the Hill three-body problem under the effect of radiation pressure of the primaries. We study the effect of the radiation parameters through the factors on the existence, position, zero-velocity curves and stability of the out-of-plane equilibrium points. These equilibrium positions are derived analytically under the action of radiation pressure exerted by the radiating primary bodies. We determined that these points emerge in symmetrical pairs, and based on the values of the radiation parameters, there may be two along the axis and either none or two on the plane (outside the axes). A thorough numerical investigation found that both radiation factors have a strong influence on the position of the out-of-plane equilibrium points. Our results also reveal that the parameters have impact on the geometry of the zero-velocity curves. Furthermore, the stability of these points is examined in the linear sense. To do so, the spatial distribution of the eigenvalues on the complex plane of the linearized system is visualized for a wide range of radiation parameter combinations. By a numerical investigation, it is found that all equilibrium points are unstable in general.Open AccessOut-of-Plane Equilibrium Points in the Photogravitational Hill Three-Body Problem
This paper investigates the movement of a negligible mass body (third body) in the vicinity of the out-of-plane equilibrium points of the Hill three-body problem under the effect of radiation pressure of the primaries. We study the effect of the radiation parameters through the factors on the existence, position, zero-velocity curves and stability of the out-of-plane equilibrium points. These equilibrium positions are derived analytically under the action of radiation pressure exerted by the radiating primary bodies. We determined that these points emerge in symmetrical pairs, and based on the values of the radiation parameters, there may be two along the axis and either none or two on the plane (outside the axes). A thorough numerical investigation found that both radiation factors have a strong influence on the position of the out-of-plane equilibrium points. Our results also reveal that the parameters have impact on the geometry of the zero-velocity curves. Furthermore, the stability of these points is examined in the linear sense. To do so, the spatial distribution of the eigenvalues on the complex plane of the linearized system is visualized for a wide range of radiation parameter combinations. By a numerical investigation, it is found that all equilibrium points are unstable in general. - Open Access
- 28 October 2023
- Published by Federal University Dutsin-Ma in FUDMA JOURNAL OF SCIENCES
- Vol. 7 (5) , 54-63
EQUILIBRIUM POINTS IN THE CR3BP OF THREE OBLATE BODIES UNDER THE EFFECTS OF CIRCUMBINARY DISC AND RADIATING PRIMARIES WITH POYNTING-ROBERTSON DRAG
We study numerically the generalized planar photogravitational circular restricted three-body problem, where an infinitesimal body is moving under the Newtonian gravitational attraction of two bodies which are finite, moving in circles around their center of mass fixed at the origin of the coordinate system, where both bodies are situated on the horizontal -axis. The third body is significantly smaller compared to the masses of the two bodies (primaries) where its influence on them can be neglected. The three participating bodies are modeled as oblate spheroids, under effect of radiation of the two main masses together with effective Poynting-Robertson drag and both of them are enclosed by a belt of homogeneous circular cluster of material points. In this paper, the existence and location of the equilibrium points and their linear stability are explored for various combinations of the model’s parameters. We observe that under constant P–R drag effect, collinear equilibrium solutions cease to exist but there are in the absence of the drag forces. We found that five or seven non-collinear equilibrium points may lie on the plane of primaries motion depends on the particular values of model’s parameters, and it is seen that the perturbing forces have significant effects on their positions and linear stability. In our model, the binary system Kruger 60 is used, and it is found that the positions of the equilibria and their stability are affected by these perturbing forces. In the case where seven critical points exist, all the equilibria are...
- 28 October 2023
- Published by Federal University Dutsin-Ma in FUDMA JOURNAL OF SCIENCES
- Vol. 7 (5) , 54-63
Open AccessEQUILIBRIUM POINTS IN THE CR3BP OF THREE OBLATE BODIES UNDER THE EFFECTS OF CIRCUMBINARY DISC AND RADIATING PRIMARIES WITH POYNTING-ROBERTSON DRAG
We study numerically the generalized planar photogravitational circular restricted three-body problem, where an infinitesimal body is moving under the Newtonian gravitational attraction of two bodies which are finite, moving in circles around their center of mass fixed at the origin of the coordinate system, where both bodies are situated on the horizontal -axis. The third body is significantly smaller compared to the masses of the two bodies (primaries) where its influence on them can be neglected. The three participating bodies are modeled as oblate spheroids, under effect of radiation of the two main masses together with effective Poynting-Robertson drag and both of them are enclosed by a belt of homogeneous circular cluster of material points. In this paper, the existence and location of the equilibrium points and their linear stability are explored for various combinations of the model’s parameters. We observe that under constant P–R drag effect, collinear equilibrium solutions cease to exist but there are in the absence of the drag forces. We found that five or seven non-collinear equilibrium points may lie on the plane of primaries motion depends on the particular values of model’s parameters, and it is seen that the perturbing forces have significant effects on their positions and linear stability. In our model, the binary system Kruger 60 is used, and it is found that the positions of the equilibria and their stability are affected by these perturbing forces. In the case where seven critical points exist, all the equilibria are...
- Open Access
- 8 July 2023
- Published by Federal University Dutsin-Ma in FUDMA JOURNAL OF SCIENCES
- Vol. 7 (3) , 110-121
MOTION AROUND THE EQUILIBRIUM POINTS IN THE PHOTOGRAVITATIONAL R4BP UNDER THE EFFECT OF CIRCUMSTELLAR BELT
In the present work, we study numerically the motion of an infinitesimal fourth body near the equilibrium points (EPs) of the photogravitational restricted four-body problem (Lagrangian configuration) under the effect of circumstellar belt. We consider the case where three the bodies of masses and (primaries) are sources of radiation as well as enclosed by a circumstellar belt and two of the primaries, and, have equal masses () and equal radiation factors () while the dominant primary body is of mass Firstly, these equilibria are determined and then the influence of the system parameters on their positions and stability is performed. In addition, the numerical exploration is performed using the Ross 104-Ross775a-Ross775b stellar system to compute the locations of the equilibria and the eigenvalues of the characteristic equation. For this system where the value of the mass parameter is beyond Routh’s value, we observe that they may be ten (four collinear and six non-collinear) or eight (two collinear and six non-collinear) EPs depending on the mass of the circumstellar belt. The linear stability of each equilibrium point is also studied and it is found that in the case where ten equilibria exist, the new collinear point, is always linearly stable while the other nine equilibria are always linearly unstable. In the case where eight equilibria exist, all of them are always linearly unstable. The zero velocity surfaces for the stellar system are drawn and regions of motion are analyzed for increasing values of the mass belt.
- 8 July 2023
- Published by Federal University Dutsin-Ma in FUDMA JOURNAL OF SCIENCES
- Vol. 7 (3) , 110-121
Open AccessMOTION AROUND THE EQUILIBRIUM POINTS IN THE PHOTOGRAVITATIONAL R4BP UNDER THE EFFECT OF CIRCUMSTELLAR BELT
In the present work, we study numerically the motion of an infinitesimal fourth body near the equilibrium points (EPs) of the photogravitational restricted four-body problem (Lagrangian configuration) under the effect of circumstellar belt. We consider the case where three the bodies of masses and (primaries) are sources of radiation as well as enclosed by a circumstellar belt and two of the primaries, and, have equal masses () and equal radiation factors () while the dominant primary body is of mass Firstly, these equilibria are determined and then the influence of the system parameters on their positions and stability is performed. In addition, the numerical exploration is performed using the Ross 104-Ross775a-Ross775b stellar system to compute the locations of the equilibria and the eigenvalues of the characteristic equation. For this system where the value of the mass parameter is beyond Routh’s value, we observe that they may be ten (four collinear and six non-collinear) or eight (two collinear and six non-collinear) EPs depending on the mass of the circumstellar belt. The linear stability of each equilibrium point is also studied and it is found that in the case where ten equilibria exist, the new collinear point, is always linearly stable while the other nine equilibria are always linearly unstable. In the case where eight equilibria exist, all of them are always linearly unstable. The zero velocity surfaces for the stellar system are drawn and regions of motion are analyzed for increasing values of the mass belt.