Multiple origins of asteroid pairs

Jacobson, Seth A.

doi:10.1017/s1743921315009655

Cited by 2 publications

(3 citation statements)

References 48 publications

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“…At the end of a binary system's lifetime, the binary disrupts forming a re-shaped asteroid, if the BYORP effect is contractive, or an asteroid pair, if the BYORP effect is expansive. Here, we assert that the BYORP effect can expand the mutual orbit to the Hill sphere creating an as-yet-unobserved population of asteroid pairs (Jacobson, 2015). However, it is possible that solar perturbations or libration growth due to the adiabatic invariant relationship between libration and mean motion de-synchronize the synchronous binary member, which is undergoing the BYORP effect (Jacobson et al, 2014b).…”

Section: Binary Asteroid Evolutionmentioning

confidence: 77%

Matching asteroid population characteristics with a model constructed from the YORP-induced rotational fission hypothesis

Jacobson

Marzari

Rossi

et al. 2016

Icarus

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From the results of a comprehensive asteroid population evolution model, we conclude that the YORP-induced rotational fission hypothesis can be consistent with the observed population statistics of small asteroids in the main belt including binaries and contact binaries. The foundation of this model is the asteroid rotation model of Marzari et al. (2011), which incorporates both the YORP effect and collisional evolution. This work adds to that model the rotational fission hypothesis, described in detail within, and the binary evolution model of Jacobson and Scheeres (2011a,b). The asteroid population evolution model is highly constrained by these and other previous works, and therefore it has only two significant free parameters: the ratio of low to high mass ratio binaries formed after rotational fission events and the mean strength of the binary YORP (BYORP) effect.We successfully reproduce characteristic statistics of the small asteroid population: the binary fraction, the fast binary fraction, steady-state mass ratio fraction and the contact binary fraction. We find that in order for the model to best match observations, rotational fission produces high mass ratio (> 0.2) binary components with four to eight times the frequency as low mass ratio (< 0.2) components, where the mass ratio is the mass of the secondary component divided by the mass of the primary component. This is consistent with post-rotational fission binary system mass ratio being drawn from either a flat or a positive and shallow distribution, since the high mass ratio bin is four times the size of the low mass ratio bin; this is in contrast to the observed steady-state binary mass ratio, which has a negative and steep distribution. This can be understood in the context of the BYORP-tidal equilibrium hypothesis, which predicts that low mass ratio binaries survive for a significantly longer period of time than high mass ratio systems. We also find that the mean of the log-normal BYORP coefficient distribution µ B 10 −2 , which is consistent with estimates from shape modeling (McMahon and Scheeres, 2012a).

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Section: Binary Asteroid Evolutionmentioning

confidence: 77%

Matching asteroid population characteristics with a model constructed from the YORP-induced rotational fission hypothesis

Jacobson

Marzari

Rossi

et al. 2016

Icarus

Self Cite

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“…A study of these pairs (Pravec & Vokrouhlický, 2009) proved their statistical significance. Unbound pairs of asteroids have also been identified in (Pravec et al, 2010;Jacobson, 2016;Kuznetsov & Safronova, 2018). One candidate pair resides in the scattered disc (Rabinowitz et al, 2011).…”

Section: Introductionmentioning

confidence: 99%

“…Different processes can lead to the formation of pairs or groups of minor bodies with close orbits. It is collisional break-ups, rotational or thermal-stressinduced splittings, tidal disruptions, and binary dissociations (see e.g., (Benz & Asphaug, 1999;Boehnhardt, 2004;Sekanina & Chodas, 2005Bottke et al, 2006;Jacobson & Scheeres, 2011;Schunová et al, 2014;Jacobson, 2016;Vokrouhlický et al, 2017). Mean motion and secular resonances can also induce orbital coherence (see e.g.…”

Section: Introductionmentioning

confidence: 99%

Dynamic evolution of pairs of trans-Neptunian objects: the case of binary and single objects in pair

Kuznetsov¹,

Al-Shiblawi²,

Gusev³

2021

caosp

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We performed a search for pairs of trans-Neptunian objects in close orbits with semi-major axes of more than 30 AU. Distances in the space of Keplerian orbits were estimated using the Kholshevnikov metrics. Found 21 pairs of trans-Neptunian objects in which one of the components is binary, for Kholshevnikov metrics in five-dimensional space of Keplerian orbits less than 0.121 AU 1/2 . All pairs belong to cold Classical Kuiper belt objects. Based on nominal orbits, the dynamic evolution of pairs of trans-Neptunian objects in the past 10 Myr has been studied numerically. We searched for low relativevelocity close encounters between trans-Neptunian objects in pairs as well as the minima of the Kholshevnikov metrics and the convergence of the lines of nodes and apses, to estimate the age of the pairs.

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Multiple origins of asteroid pairs

Cited by 2 publications

References 48 publications

Matching asteroid population characteristics with a model constructed from the YORP-induced rotational fission hypothesis

Matching asteroid population characteristics with a model constructed from the YORP-induced rotational fission hypothesis

Dynamic evolution of pairs of trans-Neptunian objects: the case of binary and single objects in pair

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