Binary asteroid population. 3. Secondary rotations and elongations

Pravec, Petr; Scheirich, P.; Kušnirák, P.; Hornoch, K.; Galád, A.; Naidu, Shantanu P.; Pray, Donald P.; Világi, Jozef; Gajdoš, Š.; Kornoš, Leonard; Krugly, Yu. N.; Cooney, W. R.; Gross, John E.; Terrell, Dirk; Gaftonyuk, N. M.; Pollock, J. T.; Husárik, M.; Chiorny, V. G.; Stephens, Robert D.; Durkee, Russell I.; Reddy, V.; Dyvig, R.; Vraštil, J.; Žižka, Jindřich; Mottola, S.; Hellmich, S.; Oey, Julian; Benishek, Vladimir; Kryszczyńska, A.; Higgins, David; Ries, J. G.; Marchis, Franck; Baek, M.; Macomber, B.; Inasaridze, R.; Kvaratskhelia, O.; Ayvazian, V.; Rumyantsev, V.; Masi, G.; Colas, François; Lecacheux, J.; Montaigut, R.; Leroy, A.; Brown, Peter; Krzeminski, Z.; Молотов, И. Е.; Reichart, D.; Haislip, J.; Lacluyzé, A.

doi:10.1016/j.icarus.2015.12.019

Cited by 102 publications

(103 citation statements)

References 34 publications

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“…However, according to Fig.12, difference between the two is obvious for secondaries with non-negligible masses. This difference is already noticed by previous researchers in their numerical simulations (Naidu & Margot 2015;Pravec et al 2016). Here, we provide an explanation to the difference.…”

Section: Physical Interpretation Of Two Families Of Periodic Orbitssupporting

confidence: 72%

“…For a specific binary asteroid system, the larger the orbit eccentricity is, the smaller the maximum libration amplitude is. These findings can help us understand the phenomenon that synchronous binary asteroid systems generally have small orbit eccentricities (Pravec et al 2016). One remark is that in this study we only consider the mutual gravity between the two asteroids, neglecting the long-term tidal and thermal effects.…”

Section: Introductionmentioning

confidence: 89%

“…According to (Pravec et al 2016), for binary asteroid systems discovered till now the b B /a B value of the secondary is mostly in the interval 0.65 to 1, i.e., a B /b B value is in the interval 1 to 1.53. For a typical mutual distance of about 4 times the primary's radius (Walsh & Jacobson 2015) and a mass ratio of secondary to primary less than 0.2, according to Fig.4 the EPs on the secondary's long axis are stable.…”

Section: Families Of Periodic Orbits Around Equilibrium Pointsmentioning

confidence: 99%

“…Till now, only three states of binary asteroid system are confirmed (Margot et al 2015;Walsh & Jacobson 2015;Pravec et al 2016): (1) the doubly synchronous state in which both the primary and the secondary are trapped in 1:1 spin-orbit resonance; (2) the synchronous state in which only the secondary is trapped in 1:1 spin-orbit resonance;…”

Section: Introductionmentioning

confidence: 99%

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On the secondary’s rotation in a synchronous binary asteroid

Wang

Hou

2020

Monthly Notices of the Royal Astronomical Society

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This paper 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 tri-axial ellipsoid secondary. Compared with classical spin-orbit work, there are two differences: (1) Influence on the mutual orbit from the secondary's rotation is considered; (2) Instead of the Hamiltonian approach, the approach of periodic orbits is adopted. Our studies find: (1) Genealogy of the two families of periodic orbits is same as that of the families around triangular libration points in the restricted three-body problem. That is, the long-period family terminates onto 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 the classical spin-orbit theory, by equating the long-period orbit with the free libration, and by equating 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 which does not break the secondary's synchronous state. We also find the 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.

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Section: Physical Interpretation Of Two Families Of Periodic Orbitssupporting

confidence: 72%

Section: Introductionmentioning

confidence: 89%

Section: Families Of Periodic Orbits Around Equilibrium Pointsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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On the secondary’s rotation in a synchronous binary asteroid

Wang

Hou

2020

Monthly Notices of the Royal Astronomical Society

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“…This is important, because the secondary fission hypothesis suggests that most low mass ratio binaries formed via this process (Jacobson and Scheeres 2011a). Indeed, two such systems have already been discovered: 3749 Balam is a triple system with an associated pair member (Vokrouhlický 2009) and 8306 Shoko is a binary system with an associated pair member (Pravec et al 2013). The creation of these binary systems simultaneously with their pair members means that binary evolution can be tied to a well estimated timescale.…”

Section: Asteroid Pair Formation After a Secondary Fission Eventmentioning

confidence: 99%

Multiple origins of asteroid pairs

Jacobson

2015

Proc. IAU

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Abstract. Rotationally fissioned asteroids produce unbound asteroid pairs that have very similar heliocentric orbits. Backward integration of their current heliocentric orbits provides an age of closest proximity that can be used to date the rotational fission event. Most asteroid pairs follow a predicted theoretical relationship between the primary spin period and the mass ratio of the two pair members that is a direct consequence of the YORP-induced rotational fission hypothesis. If the progenitor asteroid has strength, asteroid pairs may have higher mass ratios or faster rotating primaries. However, the process of secondary fission leaves the originally predicted trend unaltered. We also describe the characteristics of pair members produced by four alternative routes from a rotational fission event to an asteroid pair. Unlike direct formation from the event itself, the age of closest proximity of these pairs cannot generally be used to date the rotational fission event since considerable time may have passed.

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Spin-orbit coupling dynamics in a planar synchronous binary asteroid

Li,

Tan,

Hou

2024

Astrophys Space Sci

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Purpose: The 1:1 spin-orbit resonance phenomenon is widely observed in binary asteroid systems. We aim to investigate the intrinsic dynamic mechanism behind the phenomenon under the coupled influence of the secondary's rotation and orbital motion. Methods: The planar sphereellipsoid model is used to approximate the synchronous binary asteroid. To solve this strongly nonlinear problem, a novel algorithm based on the Lindstedt-Poincaré (LP) method is proposed to find the explicit solution of the quasi-periodic motion. Results: Numerical simulations for the Didymos system show that the high-order solution is accurate enough to provide the initial orbital conditions for further dynamic study. With the help of the solution, we compute the stable region for the synchronous state, the contour maps of the Lyapunov characteristic exponent, and the resonance curves of the basic frequencies in the parameter space. Conclusion: The stable synchronous state requires a small eccentricity e of the mutual orbit but permits a large libration angle θ of the secondary. The anti-correlation of θ and e is confirmed. The sable region for a very elongated secondary is small, which explains the lack of such secondaries in observations (see table 1 in Pravec et al ( 2016)). In addition, the findings of this research Article Title provide insights into chaos and the resonances of basic frequencies, which may play an important role in the evolution of a binary asteroid.

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Binary asteroid population. 3. Secondary rotations and elongations

Cited by 102 publications

References 34 publications

On the secondary’s rotation in a synchronous binary asteroid

On the secondary’s rotation in a synchronous binary asteroid

Multiple origins of asteroid pairs

Spin-orbit coupling dynamics in a planar synchronous binary asteroid

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