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

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 Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations

2019 ◽  
Vol 631 ◽  
pp. A149
Author(s):  
A. Rożek ◽  
S. C. Lowry ◽  
M. C. Nolan ◽  
P. A. Taylor ◽  
L. A. M. Benner ◽  
...  
Keyword(s):  
Physical Model ◽  
Spin State ◽  
Rotation Period ◽  
Optical Observations ◽  
Shape Model ◽  
Optical Photometry ◽  
Binary Asteroid ◽  
Radar Images ◽  
Yorp Effect ◽  
Contact Binary

Context. The potentially hazardous asteroid (85990) 1999 JV6 has been a target of previously published thermal-infrared observations and optical photometry. It has been identified as a promising candidate for possible Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) effect detection. Aims. The YORP effect is a small thermal-radiation torque considered to be a key factor in spin-state evolution of small Solar System bodies. In order to detect YORP on 1999 JV6 we developed a detailed shape model and analysed the spin-state using both optical and radar observations. Methods. For 1999 JV6, we collected optical photometry between 2007 and 2016. Additionally, we obtained radar echo-power spectra and imaging observations with Arecibo and Goldstone planetary radar facilities in 2015, 2016, and 2017. We combined our data with published optical photometry to develop a robust physical model. Results. We determine that the rotation pole resides at negative latitudes in an area with a 5° radius close to the south ecliptic pole. The refined sidereal rotation period is 6.536787 ± 0.000007 h. The radar images are best reproduced with a bilobed shape model. Both lobes of 1999 JV6 can be represented as oblate ellipsoids with a smaller, more spherical component resting at the end of a larger, more elongated component. While contact binaries appear to be abundant in the near-Earth population, there are only a few published shape models for asteroids in this particular configuration. By combining the radar-derived shape model with optical light curves we determine a constant-period solution that fits all available data well. Using light-curve data alone we determine an upper limit for YORP of 8.5 × 10−8 rad day−2. Conclusions. The bifurcated shape of 1999 JV6 might be a result of two ellipsoidal components gently merging with each other, or a deformation of a rubble pile with a weak-tensile-strength core due to spin-up. The physical model of 1999 JV6 presented here will enable future studies of contact binary asteroid formation and evolution.

Radar observations and a physical model of contact binary Asteroid 4486 Mithra

Icarus ◽  
2010 ◽  
Vol 208 (1) ◽  
pp. 207-220 ◽  
Author(s):  
Marina Brozovic ◽  
Lance A.M. Benner ◽  
Christopher Magri ◽  
Steven J. Ostro ◽  
Daniel J. Scheeres ◽  
...  
Keyword(s):  
Physical Model ◽  
Radar Observations ◽  
Binary Asteroid ◽  
Contact Binary

Spacecraft trajectory tracking and parameter estimation around a splitting contact binary asteroid

2020 ◽  
Vol 171 ◽  
pp. 280-289
Author(s):  
Tiago M. Silva ◽  
Jean-Baptiste Bouvier ◽  
Kathleen Xu ◽  
Masatoshi Hirabayashi ◽  
Koki Ho
Keyword(s):  
Parameter Estimation ◽  
Trajectory Tracking ◽  
Binary Asteroid ◽  
Spacecraft Trajectory ◽  
Contact Binary

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

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
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