Stability and evolution of orbits around the binary asteroid 175706 (1996 FG3): Implications for the MarcoPolo-R mission

Hußmann, H.; Oberst, J.; Wickhusen, Kai; Shi, Xian; Damme, Friedrich; Lüdicke, Fabian; Lupovka, V.; Bauer, Sven

doi:10.1016/j.pss.2012.04.010

Cited by 22 publications

(9 citation statements)

References 25 publications

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“…Recent spectral observations of some asteroids in the spheroidal class have clearly shown a large degree of spectral heterogeneity. A clear and significant example of this is asteroid 1996 FG3, which was subject to multiple observations at several epochs due to its prior interest as a rendezvous destination for space missions [19,51,1]. The data on this body show that it has a spheroidal primary and that it is currently spinning at a rapid rate, with an estimated ω ∼ 0.87 [54].…”

Section: Exposure Of Sub-surface Materialsmentioning

confidence: 99%

Landslides and Mass shedding on spinning spheroidal asteroids

Scheeres

2015

Icarus

109

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Conditions for regolith landslides to occur on spinning, gravitating spheroidal asteroids and their aftermath are studied. These conditions are developed by application of classical granular mechanics stability analysis to the asteroid environment. As part of our study we determine how slopes evolve across the surface of these bodies as a function of spin rate, the dynamical fate of material that exceeds the angle of repose, and an analysis of how the shape of the body may be modified based on these results. We find specific characteristics for body surfaces and shapes when spun near the surface disruption limit and develop what their observable implications are. The small, oblate and rapidly spinning asteroids such as 1999 KW4 Alpha and 2008 EV5 exhibit some of these observable traits. The detailed mechanisms outlined here can also provide insight and constraints on the recently observed active asteroids such as P/2013 P5, and the creation of asteroidal meteor streams.

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Section: Exposure Of Sub-surface Materialsmentioning

confidence: 99%

Landslides and Mass shedding on spinning spheroidal asteroids

Scheeres

2015

Icarus

109

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“…Scheeres (2007) studied the dynamics of contact binary asteroids, describing the minimum energy configurations as a function of the total angular momentum. Hussmann et al (2012) investigated the stability of orbits around the MarcoPolo-R target asteroids, the binary asteroid 175706 (1996 FG3), with complex gravity fields perturbed by solar radiation pressure. The authors modelled the gravity field as a homogeneous tri-axial ellipsoidal harmonic expansion up to fourth-degree and order.…”

Section: Introductionmentioning

confidence: 99%

Analysis of the orbital stability close to the binary asteroid (90) Antiope

Aljbaae

Prado

Sanchez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We provide a generalized discussion on the dynamics of a spacecraft around the equal-mass binary asteroid (90) Antiope, under the influence of solar radiation pressure at the perihelion and aphelion distances of the asteroid from the Sun. The polyhedral shape of the components of this asteroid is used to accurately model the gravitational field. Five unstable equilibrium points are determined and classified into two cases that allow classifying of the motion associated with the target as always unstable. The dynamical effects of the mass ratio of our binary system are investigated. We tested massless particles initially located at the periapsis distance on the equatorial plane of the primary of our binary asteroid. Bounded orbits around our system are not found for the longitudes λ ∈ {60, 90, 120, 240, 270, 300}. We also discuss the orbital dynamics in the full potential field of (90) Antiope. The tested motions are mainly dominated by the binary’s gravitational field; no significant effects of the SRP are detected. For λ = 180°, less perturbed orbits are identified between 420 and 700 km from the centre of the system, that corresponds to orbits with Δa < 30 km and Δe < 0.15. All the orbits with initial periapsis distance smaller than 350 km either collide with components of our asteroid or escape from the system.

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“…Nevertheless, Scheeres et al (2006) have shown that, for a body smaller than few kilometres, like asteroid (25143) Itokawa, the solar radiation pressure parameter become relevant even in close proximity to the body. Moreover, in the Hill problem, the influence of solar radiation pressure can lead to both unstable and stable spacecraft orbits near bodies with a diameter smaller than few kilometres (Hussmann et al 2012). However, the solar radiation pressure model, as well as the eclipse model around rotating asteroids, were only recently presented in Xin et al (2016).…”

Section: Introductionmentioning

confidence: 99%

Dynamics in the vicinity of (101955) Bennu: solar radiation pressure effects in equatorial orbits

Chanut

Aljbaae

Prado

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Here we study the dynamical effects of the solar radiation pressure (SRP) on a spacecraft that will survey the near-Earth rotating asteroid (101955) Bennu when the projected shadow is accounted for. The spacecraft's motion near (101955) Bennu is modelled in the rotating frame fixed at the centre of the asteroid, neglecting the sun gravity effects. We calculate the solar radiation pressure at the perihelion, semi-major axis and aphelion distances of the asteroid from the Sun. The goals of this work are to analyse the stability for both homogeneous and inhomogeneous mass distribution and study the effects of the solar radiation pressure in equatorial orbits close to the asteroid (101955) Bennu. As results, we find that the mascon model divided into ten equal layers seems to be the most suitable for this problem. We can highlight that the centre point E8, which was linearly stable in the case of the homogeneous mass distribution, becomes unstable in this new model changing its topological structure. For a Sun initial longitude ψ 0 = −180 o , starting with the spacecraft longitude λ = 0, the orbits suffer fewer impacts and some (between 0.4 and 0.5 km), remaining unwavering even if the maximum solar radiation is considered. When we change the initial longitude of the Sun to ψ 0 = −135 o , the orbits with initial longitude λ = 90 0 appear to be more stable. Finally, when the passage of the spacecraft in the shadow is accounted for, the effects of solar radiation pressure are softened, and we find more stable orbits.

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Stability and evolution of orbits around the binary asteroid 175706 (1996 FG3): Implications for the MarcoPolo-R mission

Cited by 22 publications

References 25 publications

Landslides and Mass shedding on spinning spheroidal asteroids

Landslides and Mass shedding on spinning spheroidal asteroids

Analysis of the orbital stability close to the binary asteroid (90) Antiope

Dynamics in the vicinity of (101955) Bennu: solar radiation pressure effects in equatorial orbits

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