Resonance Occupation in the Kuiper Belt: Case Examples of the 52 and Trojan Resonances

Chiang, Eugene; Jordán, Andrés; Millis, R. L.; Buie, M. W.; Wasserman, L. H.; Elliot, J. L.; Kern, S.; Trilling, David E.; Meech, К. J.; Wagner, R. M.

doi:10.1086/375207

Cited by 139 publications

(140 citation statements)

References 37 publications

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“…3 during 1 Gyr, except Trojan 2001QR322, which escapes from the Lagrangian L 4 point after about 112 Myr. This last observation was somehow unexpected, since Chiang et al (2003) concluded that this same Neptune Trojan was stable over 1 Gyr. This difference of behaviors is a consequence of a modification in the initial conditions (Table A.3), obtained with new observational data.…”

Section: Stability Of the Neptune Trojansmentioning

confidence: 91%

Neptune Trojans and Plutinos: colors, sizes, dynamics, and their possible collisions

Almeida

Peixinho

Correia

2009

A&A

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Neptune Trojans and Plutinos are two subpopulations of trans-Neptunian objects located in the 1:1 and the 3:2 mean motion resonances with Neptune, respectively, and therefore protected from close encounters with the planet. However, the orbits of these two kinds of objects may cross very often, allowing a higher collisional rate between them than with other kinds of trans-Neptunian objects, and a consequent size distribution modification of the two subpopulations. Observational colors and absolute magnitudes of Neptune Trojans and Plutinos show that i) there are no intrinsically bright (large) Plutinos at small inclinations; ii) there is an apparent excess of blue and intrinsically faint (small) Plutinos; and iii) Neptune Trojans possess the same blue colors as Plutinos within the same (estimated) size range do. For the present subpopulations we analyzed the most favorable conditions for close encounters/collisions and address any link there could be between those encounters and the sizes and/or colors of Plutinos and Neptune Trojans. We also performed a simultaneous numerical simulation of the outer Solar System over 1 Gyr for all these bodies in order to estimate their collisional rate. We conclude that orbital overlap between Neptune Trojans and Plutinos is favored for Plutinos with large libration amplitudes, high eccentricities, and small inclinations. Additionally, with the assumption that the collisions can be disruptive creating smaller objects not necessarily with similar colors, the present high concentration of small Plutinos with small inclinations can thus be a consequence of a collisional interaction with Neptune Trojans and such hypothesis should be further analyzed.

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Section: Stability Of the Neptune Trojansmentioning

confidence: 91%

Neptune Trojans and Plutinos: colors, sizes, dynamics, and their possible collisions

Almeida

Peixinho

Correia

2009

A&A

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“…The Kuiper belt population is in turn subdivided in two sub-populations: the resonant population (star symbols in Figure 1) and the classical belt (dots). The former is made of the objects located in some major mean motion resonance with Neptune (essentially the 3:4, 2:3 and 1:2 resonances, but also the 2:5 -see Chiang et al, 2003), while the classical belt objects are not in any noticeable resonant configuration. It is well known that mean motion resonances offer a protection mechanism against close encounters with the resonant planet (Cohen and Hubbard, 1965).…”

Section: The Trans-neptunian Populationsmentioning

confidence: 99%

The Kuiper Belt and its Primordial Sculpting

Morbidelli

Brown

Levison

2003

Earth, Moon, and Planets

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Abstract. We discuss the structure of the Kuiper belt as it can be inferred from the first decade of observations. In particular, we focus on its most intriguing properties -the mass deficit, inclination distribution, the apparent existence of an outer edge and of a correlation among inclinations, colours and sizes -which clearly show that the belt has lost its pristine structure of a dynamically cold protoplanetary disk. Understanding how the Kuiper belt acquired its present structure will provide insight into the formation of the outer planetary system and on its early evolution. We outline a scenario of primordial sculpting -issued from a combination of mechanisms proposed by various authorsthat seems to explain most of the observed properties of the Kuiper belt. Several aspects are not yet totally clear. But, for the first time, we have a view -if not of the detailed sculpture -at least of its rough cast.

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“…This resonance occupancyreinforces the finding that there are many TNOs in high-order, distant > a 50 resonances (Chiang et al 2003;Lykawka & Mukai 2007a;Gladman et al 2008;2012;Alexandersen et al 2014;Pike et al 2015;Kaib & Sheppard 2016;Sheppard et al 2016). Objects in large-a resonances are inefficiently discovered due to ther 4 dependence for reflected flux, the overall steep TNO luminosity function, and because the large eccentricities of such orbits placemost of the population at large distances at any given timeand thus below the flux limit of wide-field surveys.…”

Section: Orbitmentioning

confidence: 85%

Ossos. Iv. Discovery of a Dwarf Planet Candidate in the 9:2 Resonance With Neptune

Bannister

Alexandersen

Benecchi

et al. 2016

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We report the discovery and orbit of a new dwarf planet candidate, 2015 RR 245 , by the Outer Solar System Origins Survey (OSSOS). The orbit of 2015 RR 245 is eccentric (e=0.586), with a semimajor axis near 82 au, yielding a perihelion distance of 34 au. 2015 RR 245 has -=  g r 0.59 0.11 and absolute magnitude =  H 3.6 0.1; r for an assumed albedo of p V =12%, the object has a diameter of ∼670km. Based on astrometric measurements from OSSOS and Pan-STARRS1, we find that 2015 RR 245 is securely trapped on ten-megayear timescales in the 9:2 mean-motion resonance with Neptune. It is the first trans-Neptunian object (TNO) identified in this resonance. On hundred-megayeartimescales, particles in 2015 RR 245 -like orbits depart and sometimes return to the resonance, indicating that 2015 RR 245 likely forms part of the long-lived metastable population of distant TNOs that drift between resonance sticking and actively scattering via gravitational encounters with Neptune. The discovery of a 9:2 TNO stresses the role of resonances in the long-term evolution of objects in the scattering diskand reinforces the view that distant resonances are heavily populated in the current solar system. This object further motivates detailed modeling of the transient sticking population.

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Resonance Occupation in the Kuiper Belt: Case Examples of the 52 and Trojan Resonances

Cited by 139 publications

References 37 publications

Neptune Trojans and Plutinos: colors, sizes, dynamics, and their possible collisions

Neptune Trojans and Plutinos: colors, sizes, dynamics, and their possible collisions

The Kuiper Belt and its Primordial Sculpting

Ossos. Iv. Discovery of a Dwarf Planet Candidate in the 9:2 Resonance With Neptune

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