Orbital Stability Around the Primary of a Binary Asteroid System

2021 ◽  
pp. 1-14
Author(s):  
Tao Fu ◽  
Yue Wang
Keyword(s):  
Orbital Stability ◽  
Binary Asteroid ◽  
Binary Asteroid System

scholarly journals On the secondary’s rotation in a synchronous binary asteroid

2020 ◽  
Vol 493 (1) ◽  
pp. 171-183
Author(s):  
H S Wang ◽  
X Y Hou
Keyword(s):  
Periodic Orbits ◽  
Body Problem ◽  
Spin Orbit ◽  
Binary Asteroid ◽  
Classical Spin ◽  
Long Period ◽  
Period Orbit ◽  
Short Period ◽  
Orbit Eccentricity ◽  
Binary Asteroid System

ABSTRACT This article studies the secondary’s rotation in a synchronous binary asteroid system in which the secondary enters the 1:1 spin-orbit resonance. The model used is the planar full two-body problem, composed of a spherical primary plus a triaxial ellipsoid secondary. Compared with classical spin-orbit work, there are two differences: (1) influence of the secondary’s rotation on the mutual orbit is considered and (2) instead of the Hamiltonian approach, the approach of periodic orbits is adopted. Our studies find the following. (1) The genealogy of the two families of periodic orbits is the same as that of the families around triangular libration points in the restricted three-body problem. That is, the long-period family terminates on to a short-period orbit travelling N times. (2) In the limiting case where the secondary’s mass is negligible, our results can be reduced to classical spin-orbit theory, by equating the long-period orbit with free libration and the short-period orbit with the forced libration caused by orbit eccentricity. However, the two models show obvious differences when the secondary’s mass is non-negligible. (3) By studying the stability of periodic orbits for a specific binary asteroid system, we are able to obtain the maximum libration amplitude of the secondary (which is usually less than 90°) and the maximum mutual orbit eccentricity that does not break the secondary’s synchronous state. We also find an anti-correlation between the secondary’s libration amplitude and the orbit eccentricity. The (65803) Didymos system is taken as an example to show the results.

scholarly journals Angles-Only Navigation in the Proximity of a Binary Asteroid System

2021 ◽  
Vol 44 (1) ◽  
pp. 57-74
Author(s):  
Francesco Torre ◽  
Stuart Grey ◽  
Massimiliano Vasile
Keyword(s):  
Binary Asteroid ◽  
Binary Asteroid System

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

2020 ◽  
Vol 496 (2) ◽  
pp. 1645-1654
Author(s):  
S Aljbaae ◽  
A F B A Prado ◽  
D M Sanchez ◽  
H Hussmann
Keyword(s):  
Gravitational Field ◽  
Equilibrium Points ◽  
Orbital Stability ◽  
Solar Radiation Pressure ◽  
Equal Mass ◽  
Orbital Dynamics ◽  
Full Potential ◽  
Mass Ratio ◽  
Binary Asteroid ◽  
Polyhedral Shape

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.

Stable Regions of Motion Around a Binary Asteroid System

2019 ◽  
Vol 42 (11) ◽  
pp. 2521-2531 ◽  
Author(s):  
Yuying Liang ◽  
Gerard Gómez ◽  
Josep J. Masdemont ◽  
Ming Xu
Keyword(s):  
Binary Asteroid ◽  
Binary Asteroid System

Lift-off velocity on the surface of a binary asteroid system

2020 ◽  
Vol 170 ◽  
pp. 302-319
Author(s):  
Xuewen Liu ◽  
Hongwei Yang ◽  
Shuang Li ◽  
Jun Sun
Keyword(s):  
Binary Asteroid ◽  
Binary Asteroid System ◽  
Lift Off

On the post-impact spin state of the secondary component of the Didymos-Dimorphos binary asteroid system

2020 ◽  
Author(s):  
Harrison Agrusa ◽  
Kleomenis Tsiganis ◽  
Ioannis Gkolias ◽  
Derek Richardson ◽  
Alex Davis ◽  
...  
Keyword(s):  
Spin State ◽  
Uniform Density ◽  
Dynamical Structure ◽  
Spin Orbit ◽  
Binary Asteroid ◽  
Planetary Defense ◽  
Out Of Plane ◽  
Post Impact ◽  
Binary Asteroid System ◽  
Binary Orbit

<p>NASA’s Double Asteroid Redirection Test (DART) is designed to be the first demonstration of a kinetic impactor for planetary defense against a small body impact hazard. The target is the smaller component of the Didymos-Dimorphos binary asteroid system. The DART impact will abruptly change the relative velocity of the secondary (Dimorphos), increasing the binary eccentricity and exciting librations in the secondary. The observed change in the binary orbit period will be used to infer the “beta factor”, or the momentum transfer efficiency, an important parameter used in planetary defense. The post-impact spin and librational dynamics are expected to be highly dependent on the momentum transferred to the target (i.e., beta) and the shape of the secondary, which is still unconstrained.</p> <p>In this work, we explore the possible post-impact spin state of Dimorphos, as a function of its shape and beta, assuming it has an ellipsoidal shape and that both bodies have a uniform density. We have conducted attitude dynamics simulations with a modified 3-D spin-orbit model, accounting for the secondary’s shape and the primary’s oblateness, to understand the underlying dynamical structure of the system. In addition, we have used the radar-derived polyhedral shape model of Didymos in high-fidelity Full Rigid Two-Body Problem (FR2BP) simulations to capture the fully three-dimensional nature of the problem. We consider the outcomes from a simplified planar impact, where the DART momentum is transferred within the binary orbit plane, opposite the motion of Dimorphos, in addition to a more realistic case that accounts for the full DART velocity vector (which contains out-of-plane components).</p> <p>With both simulation tools, we produce the expected signatures of the 1:1 and 2:1 secondary resonances between the free and forced libration periods, corresponding to axial ratios of a/b = 1.414 and a/b = 1.087, respectively. For moderate values of beta (~3), we find that the libration amplitude can exceed ~40 degrees in most cases. For some possible axial ratios, it is even possible to achieve a libration amplitude exceeding 40 degrees with beta values as low as 1. In addition, both codes reveal that the secondary may be attitude unstable in many cases, and can enter a chaotic tumbling state for larger values of beta (~5). In some cases, Dimorphos is able to break from its assumed 1:1 spin-orbit resonance.</p> <p>In the case with a more realistic impact geometry (where some momentum is transferred out-of-plane), the results are relatively similar. The most noticeable difference is in the cases that result in a chaotic tumbling state. In those cases, the characteristic timescale for entering the chaotic tumbling state is much shorter – typically only several orbit periods are required. We also discuss the feasibility of detecting the post-impact spin state of Dimorphos with ground-based observations.</p> <p>This study was supported in part by the DART mission, NASA Contract # NNN06AA01C to JHU/APL. The work of K.T. and I.G. is supported by the EC Horizon 2020 research and innovation programme, under grant agreement No. 870377 (project "NEO-MAPP"). Some of the simulations herein were carried out on The University of Maryland Astronomy Department’s YORP cluster, administered by the Center for Theory and Computation.</p>

scholarly journals Symbolic dynamics in a binary asteroid system

2020 ◽  
Vol 91 ◽  
pp. 105414
Author(s):  
Sara Di Ruzza ◽  
Jérôme Daquin ◽  
Gabriella Pinzari
Keyword(s):  
Symbolic Dynamics ◽  
Binary Asteroid ◽  
Binary Asteroid System

Numerical analysis of orbital motion around a contact binary asteroid system

2016 ◽  
Vol 58 (3) ◽  
pp. 387-401 ◽  
Author(s):  
Jinglang Feng ◽  
Ron Noomen ◽  
Pieter Visser ◽  
Jianping Yuan
Keyword(s):  
Numerical Analysis ◽  
Orbital Motion ◽  
Binary Asteroid ◽  
Contact Binary ◽  
Binary Asteroid System
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