Extension of the rotating dipole model with oblateness of both primaries

Zeng, Xia; Liu, Xiangdong; Li, Junfeng

doi:10.1088/1674-4527/17/1/2

Cited by 19 publications

(7 citation statements)

References 37 publications

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“…The final perturbation accounted for is the fact that the two asteroids of binary system 1999 KW4 do not satisfy the assumption of spherically shaped bodies. In particular, Table 3 shows a significant difference between the bodies' equatorial and polar radii, the effect of which can be included in the dynamics through the following perturbing potential for the oblateness of the two asteroids [39,40]:…”

Section: Oblateness Of the Binary Asteroidsmentioning

confidence: 99%

Solar-Sail Orbital Motion About Asteroids and Binary Asteroid Systems

Heiligers

Scheeres

2018

Journal of Guidance, Control, and Dynamics

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Solar radiation pressure (SRP) is a major orbital perturbation for missions to small bodies like asteroids and binary asteroid systems. This paper studies the utilization of SRP on a solar sail for asteroid mission applications, specifically to generate artificial equilibrium points (AEPs) and displaced periodic orbits in these systems. For the single asteroid case, contours of AEPs for constant sail acceleration magnitudes are found in the Hill + SRP problem as well as periodic orbits around these AEPs. The binary system is modeled by first adding a fourth-body perturbation to the Hill + SRP dynamics, demonstrating the effect of the smaller asteroid as an oscillatory motion superimposed on the unperturbed orbit. Truly periodic orbits are obtained in the bi-circular + SRP problem, showing the existence of socalled pole-sitter-like orbits above the binary system's orbital plane. Higher-fidelity dynamical effects are investigated for these pole-sitter-like orbits for binary system 1999 KW4, showing feasibility of the orbits around aphelion. All results are generated for nearterm sail technology and for a simple, fixed sail attitude relative to the Sun. They therefore = Denotes first order derivative with respect to time   = Denotes second order derivative with respect to time

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Section: Oblateness Of the Binary Asteroidsmentioning

confidence: 99%

Solar-Sail Orbital Motion About Asteroids and Binary Asteroid Systems

Heiligers

Scheeres

2018

Journal of Guidance, Control, and Dynamics

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“…As one of the important branches, periodic orbits play a significant role and are considered to be key to understanding the nature of asteroid dynamics. Therefore, various research that regards this issue has been obtained, such as gravity potential field computation [1][2][3][4][5][6][7][8], equilibrium points searching and analyses [9][10][11][12][13][14][15], 2 generation of periodic orbits [16][17][18][19][20], classification [21] and bifurcation analysis [22][23]. These outstanding studies have further contributed to the development of asteroid research and lay a firm foundation for later studies.…”

Section: Introductionmentioning

confidence: 99%

Convergence of a periodic orbit family close to asteroids during a continuation

Kang

Jiang

2020

Results in Physics

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“…Toutatis [18], 216 Kleopatra [19][20][21][22][23][24][25] and the binary near-Earth asteroid (66391) 1999 KW4 [26][27][28].…”

Section: Introductionmentioning

confidence: 99%

Stability and motion around equilibrium points in the rotating plane-symmetric potential field

et al. 2018

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This study presents a study of equilibrium points, periodic orbits, stabilities, and manifolds in a rotating plane-symmetric potential field. It has been found that the dynamical behaviour near equilibrium points is completely determined by the structure of the submanifolds and subspaces. The non-degenerate equilibrium points are classified into twelve cases. The necessary and sufficient conditions for linearly stable, non-resonant unstable and resonant equilibrium points are established. Furthermore, the results show that a resonant equilibrium point is a Hopf bifurcation point. In addition, if the rotating speed changes, two non-degenerate equilibria may collide and annihilate each other. The theory developed here is lastly applied to two particular cases, motions around a rotating, homogeneous cube and the asteroid 1620 Geographos. We found that the mutual annihilation of equilibrium points occurs as the rotating speed increases, and then the first surface shedding begins near the intersection point of the -x axis and the surface. The results can be applied to planetary science, including the birth and evolution of the minor bodies in the Solar system, the rotational breakup and surface mass shedding of asteroids, etc.

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Extension of the rotating dipole model with oblateness of both primaries

Cited by 19 publications

References 37 publications

Solar-Sail Orbital Motion About Asteroids and Binary Asteroid Systems

Solar-Sail Orbital Motion About Asteroids and Binary Asteroid Systems

Convergence of a periodic orbit family close to asteroids during a continuation

Stability and motion around equilibrium points in the rotating plane-symmetric potential field

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