The motion properties of the infinitesimal body in the framework of bicircular Sun perturbed Earth–Moon system

The aim of the present paper is to analyze the viability of using Lorentz Force (LF) acting on a charged spacecraft to neutralize the effects of Solar Radiation Pressure (SRP) on the longitude of the ascending node and the argument of perigee of the spacecraft’s orbit. In this setting, the Gauss planetary equations for LF and SRP are presented and averaged over the true anomaly. The averaged variations for the longitude of the ascending node (h) and the argument of perigee (g) are invariant under the symmetry (i,g)⟶(−i,−g) due to Lorentz Force. The sum of change rates due to both perturbing forces of LF and SRP is assigned by zero to estimate the charge amount to balance the variation for the argument of perigee and longitude of ascending. Numerical investigations have been developed to show the evolution of the charge quantity for different orbital parameters at both Low Earth and Geosynchronous Orbits.

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“…Compiling Equations (10)- (12) with Equation (9), then we can evaluate the components of SRP for practical applications.…”

Section: Effect Of Solar Radiation Pressurementioning

confidence: 99%

“…They also used Lie transformation to eliminate the expressions, which involve inclination terms during the obtainment of required solutions. But the effect of non-sphericity and SRP are also studied within the framework of two and three bodies problem, for details see for instance [8][9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

Controlling the Perturbations of Solar Radiation Pressure on the Lorentz Spacecraft

et al. 2020

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“…(see Cronin et al (1964)). Abouelmagd and Ansari (2019) revealed the motion properties of the infinitesimal body in the framework of Bi-Circular Sun perturbed Earth-Moon System. Singh and Omale (2020) did a study on the Bi-Circular R4BP with dissipative forces and they pointed that the P-R drag exert greater drag effect on the motion of a test particle than the Stokes drag.…”

Section: Introductionmentioning

confidence: 99%

Equilibria, stability and chaos in photogravitational Bi-Circular restricted four-body problem

Singh

Omale

2021

Heliyon

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“…ey noticed that collinear points are always unstable, while triangular points are stable for certain interval of the mass ratio. Abouelmagd and Ansari [25] studied numerically the bicircular Sun perturbed Earth-Moon-satellite system and illustrated the equilibrium points, Poincaré's surfaces sections, and basins of attracting domain.…”

Section: Introductionmentioning

confidence: 99%

Motion of the Infinitesimal Variable Mass in the Generalized Circular Restricted Three-Body Problem under the Effect of Asteroids Belt

Bouaziz-Kellil

2020

Advances in Astronomy

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The present paper deals with the study of the motion’s properties of the infinitesimal variable mass body moving in the same orbital plan as two massive bodies (considered as primaries). It is assumed that the massive bodies have radiating effects, have oblate shapes, and are moving in circular orbits around their common center of mass. Using the procedures established by Singh and Abouelmagd, we determined the equations of motion of the infinitesimal body for which we assumed that under the effects of radiation and oblateness of the primaries, its mass varies following Jean’s law. We evaluated analytically and numerically the locations of equilibrium points and examined the stability of these equilibrium points. Finally, we found that all the points are unstable.

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The motion properties of the infinitesimal body in the framework of bicircular Sun perturbed Earth–Moon system

Cited by 40 publications

References 19 publications

Controlling the Perturbations of Solar Radiation Pressure on the Lorentz Spacecraft

Controlling the Perturbations of Solar Radiation Pressure on the Lorentz Spacecraft

Equilibria, stability and chaos in photogravitational Bi-Circular restricted four-body problem

Motion of the Infinitesimal Variable Mass in the Generalized Circular Restricted Three-Body Problem under the Effect of Asteroids Belt

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