Surface motion relative to the irregular celestial bodies

Jiang, Yu; Zhang, Yun; Baoyin, Hexi

doi:10.1016/j.pss.2016.04.007

Cited by 25 publications

(9 citation statements)

References 41 publications

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“…In this study, an effective, parallel, three-dimensional N-body numerical code, Discrete Element Method (DEM) 10 , 20 , 39 , in which elastic spherical particles (i.e., soft-sphere) are described by linear-spring dashpot in conjunction with slider model, is carried out to simulate the impact process of various projectiles into granular regolith based on our previous work 40 . The motion of each particles is simultaneously calculated by taking into account whole mechanical interactions that occur when particles make contact, such as various kinds of friction, including rolling friction, which corresponds to the transformation of rotation energy into friction energy, and the normal and tangential deformation of colliding particles.…”

Section: Methodsmentioning

confidence: 99%

Asteroid surface impact sampling: dependence of the cavity morphology and collected mass on projectile shape

Cheng

Baoyin

2017

Sci Rep

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In-situ exploration and remote thermal infrared observation revealed that a large fraction of Solar System small bodies should be covered with granular regolith. The complex and varied geology of the regolith layer may preserve the historical records of the surface modification and topographic evolution experienced by asteroids, especially cratering processes, in which the projectile shape plays a crucial role. Regarding the impact sampling scheme, the projectile-shape dependence of both the cavity morphology and the collected mass remains to be explored. This paper studies the process of the low-speed impact sampling on granular regolith using projectiles of different shapes. The results demonstrate that the projectile shape significantly influences the excavation stage, forming cavities with different morphologies, i.e., cone-shaped, bowl-shaped and U-shaped. We further indicate that the different velocity distributions of the ejecta curtains due to the various projectile shapes result in various amounts of collected mass in sampler canister, regarding which the 60° conical projectile exhibits preferable performance for impact sampling scheme. The results presented in this article are expected to reveal the dependence of the excavation process on projectile shape under micro gravity and provide further information on the optimal designs of impact sampling devices for future sample-return space missions.

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Section: Methodsmentioning

confidence: 99%

Asteroid surface impact sampling: dependence of the cavity morphology and collected mass on projectile shape

Cheng

Baoyin

2017

Sci Rep

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“…Here λ represents the eigenvalues of the equilibrium point. There are several topological cases for the equilibrium point (Jiang et al 2016c). The most common cases are ordinary case O1, O2, O3 and O4.…”

Section: Gravitational Potential and Effective Potentialmentioning

confidence: 99%

The dynamical environment of the primary in the triple asteroid (45) Eugenia

Jiang

2020

Open Astronomy

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We investigated the dynamical behavior in the potential of the primary in the triple asteroid (45) Eugenia with the calculation of the full gravitational potential caused by its 3D irregular shape. We presented the whole structure of the gravitational potential and the effective potential of (45) Eugenia in the coordinate planes, and showed the surface height, surface gravitational force accelerations, and the surface effective potential. The surface gravitational environment has been discussed. The zero-velocity curves and the position of external equilibrium points are calculated and showed relative to the 3D shape of the asteroid to help compare the relationship of the characteristic of the gravitational potential and the shape of the asteroid. There are five equilibrium points in the gravitational potential (45) Eugenia. We presented the positions, eigenvalues, topological cases, and stability of these equilibrium points. To analyze the variety of the orbital parameters close to (45) Eugenia, we computed two different orbits and compared the results. The mechanical energy, the semi-major axis, and the eccentricity have two different periods: the long period and the short period. The inclination have three different periods, an intermediate period is occurred. The longitude of the ascending node and the argument of periapsis not only have two periodic terms, but also have a secular term.

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“…The shape and gravitational model of minor celestial bodies can be modeled by the polyhedral model [3,[25][26][27] or the hard/soft-sphere discrete element method [10,[28][29][30]. Asteroid 433 Eros is elongated, and has both concave and convex areas on surface.…”

Section: Gravitational Potentialmentioning

confidence: 99%

Stable periodic orbits for spacecraft around minor celestial bodies

Jiang

Schmidt

et al. 2017

Astrodyn

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We are interested in stable periodic orbits for spacecraft in the gravitational field of minor celestial bodies. The stable periodic orbits around minor celestial bodies are useful not only for the mission design of the deep space exploration, but also for studying the long-time stability of small satellites in the large-size-ratio binary asteroids. The irregular shapes and gravitational fields of the minor celestial bodies are modeled by the polyhedral model.Using the topological classifications of periodic orbits and the grid search method, the stable periodic orbits can be calculated and the topological cases can be determined. Furthermore, we find five different types of stable periodic orbits around minor celestial bodies: (1) stable periodic orbits generated from the stable equilibrium points outside the minor celestial body; (2) stable periodic orbits continued from the unstable periodic orbits around the

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Surface motion relative to the irregular celestial bodies

Cited by 25 publications

References 41 publications

Asteroid surface impact sampling: dependence of the cavity morphology and collected mass on projectile shape

Asteroid surface impact sampling: dependence of the cavity morphology and collected mass on projectile shape

The dynamical environment of the primary in the triple asteroid (45) Eugenia

Stable periodic orbits for spacecraft around minor celestial bodies

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