Trans-Neptunian Objects Transiently Stuck in Neptune’s Mean-motion Resonances: Numerical Simulations of the Current Population

Yu, Tze Yeung Mathew; Murray-Clay, Ruth; Volk, Kathryn

doi:10.3847/1538-3881/aac6cd

Cited by 36 publications

(68 citation statements)

References 35 publications

(75 reference statements)

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“…In the specific case of the resonance 1:2, the closest resonance with some, though tiny, dynamical traces seems to be 15:29. Yu et al (2018) performed numerical integrations of particles with 30 < a < 100 au looking for captures in MMRs and they obtained a very illustrative map of captures for resonances k p :k (q:p using their notation) that shows that the efficiency of captures drops substantially for k p > 13 in very good agreement with our results. It is worth mentioning that Chambers (1997) studied the credibility of exterior MMRs with Jupiter and concluded that for high k/k p ratios the binding energies of the comets to the Sun are not large enough to overcome the planetary perturbations and the resonances cannot work.…”

Section: On the Existence Of High K P :K Resonancessupporting

confidence: 80%

Three-dimensional structure of mean motion resonances beyond Neptune

Gallardo

2020

Celest Mech Dyn Astr

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We propose a semianalytical method for the calculation of widths, libration centers and small amplitude libration periods of the mean motion resonances k p :k in the framework of the circular restricted three body problem valid for arbitrary eccentricities and inclinations. Applying the model to the trans Neptunian region (TNR) we obtain several atlas of resonances between 30 and 100 au showing their domain in the plane (a, e) for different orbital inclinations. The resonance width may change substantially when varying the argument of the perihelion of the resonant object and in order to take into account these variations we introduce the concept of resonance fragility. Resonances 1:k and 2:k are the widest, strongest, most isolated ones and with lower fragility for all interval of inclinations and eccentricities. We discuss about the existence of high k p :k resonances. We analyze the distribution of the resonant populations inside resonances 1:1, 2:3, 3:5, 4:7, 1:2 and 2:5. We found that the populations are in general located near the regions of the space (e, i) where the resonances are wider and less fragile with the notable exception of the population inside the resonance 4:7 and in a lesser extent the population inside 3:5 which are shifted to lower eccentricities.

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Section: On the Existence Of High K P :K Resonancessupporting

confidence: 80%

Three-dimensional structure of mean motion resonances beyond Neptune

Gallardo

2020

Celest Mech Dyn Astr

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“…The resonance sticking mechanism was first noticed by Duncan and Levison (1997) and since then is has been studied by a number of authors. In particular, it was found for objects in Neptune encountering orbits (scattered TNOs) (Lykawka and Mukai 2007;Yu et al 2018), and in the temporarily capture of Uranian and Neptune Trojans from the dynamical evolution of Centaurs (Alexandersen et al 2013). We note several resonance captures in the whole evolution with a tendency of GPCs to be captured into MMR with Neptune: 1:1, 3:2, 2:1 and 3:1 and 5:2.…”

Section: Dynamical Evolution Of Observed Gpcmentioning

confidence: 58%

“…In particular, Lykawka and Mukai (2007) found that evolution of scattered TNOs is described by multiple temporary resonance sticking and continuous scattering by Neptune and that this mechanism is relevant mostly at a < 250 au, consistent with our result. Yu et al (2018) predicted that the current transient-sticking population comprises 40% of the total transiently stuck + scattering TNOs, and therefore is a very important mechanism in the SD zone.…”

Section: Dynamical Evolutionmentioning

confidence: 99%

Centaur and giant planet crossing populations: origin and distribution

Sisto

Rossignoli

2020

Celest Mech Dyn Astr

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The current giant planet region is a transitional zone where transneptunian objects (TNOs) cross in their way to becoming Jupiter Family Comets (JFCs). Their dynamical behavior is conditioned by the intrinsic dynamical features of TNOs and also by the encounters with the giant planets. We address the Giant Planet Crossing (GPC) population (those objects with 5.2 au < q < 30 au) studying their number and their evolution from their sources, considering the current configuration of the Solar System. This subject is reviewed from previous investigations and also addressed by new numerical simulations of the dynamical evolution of Scattered Disk Objects (SDOs). We obtain a model of the intrinsic orbital element distribution of GPCs. The Scattered Disk represents the main source of prograde GPCs and Centaurs, while the contribution from Plutinos lies between one and two orders of magnitude below that from the SD. We obtain the number and size distribution of GPCs from our model, computing 9600 GPCs from the SD with D > 100 km and ∼ 10 8 with D > 1 km in the current population. The contribution from other sources is considered negligible. The mean lifetime in the Centaur zone is 7.2 Myr, while the mean lifetime of SDOs in the GPC zone is of 68 Myr. The latter is dependent on the initial inclination, being the ones with high inclinations the ones that survive the longest in the GPC zone. There is also a correlation of lifetime with perihelion distance, where greater perihelion leads to longer lifetime. The dynamical evolution of observed GPCs is different for prograde and retrograde objects. Retrograde GPCs have lower median lifetime than prograde ones, thus experiencing a comparatively faster evolution. However, it is probable that this faster evolution is due to the fact that the majority of retrograde GPCs have low perihelion values and then, lower lifetimes.

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“…RTNOs show dynamical characteristics (e.g., inclination distribution) different from those of the classical Kuiper belt, but may be connected to the scattered disk population (Gomes et al 2008), objects on high eccentricity orbits with perihelia beyond Neptune, and semi-major axes beyond the 2:1 resonance. Recent studies (Yu et al 2018) indicate that a significant fraction of all scattered objects are transiently stuck in mean motion resonances, suggesting that these objects originated from the same single population.…”

Section: Introductionmentioning

confidence: 99%

“TNOs are Cool”: A survey of the trans-Neptunian region

Farkas-Takács

Kiss

Vilenius

et al. 2020

A&A

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The goal of this work is to determine the physical characteristics of resonant, detached and scattered disk objects in the trans-Neptunian region, observed mainly in the framework of the “TNOs are Cool” Herschel open time key programme. Based on thermal emission measurements with the Herschel/PACS and Spitzer/MIPS instruments, we determine size, albedo, and surface thermal properties for 23 objects using radiometric modeling techniques. This is the first analysis in which the physical properties of objects in the outer resonances are determined for a notable sample. In addition to the results for individual objects, we compared these characteristics with the bulk properties of other populations of the trans-Neptunian region. The newly analyzed objects show a large variety of beaming factors, indicating a diversity of thermal properties, and in general they follow the albedo-color clustering identified earlier for Kuiper belt objects and Centaurs, further strengthening the evidence for a compositional discontinuity in the young Solar System.

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Trans-Neptunian Objects Transiently Stuck in Neptune’s Mean-motion Resonances: Numerical Simulations of the Current Population

Cited by 36 publications

References 35 publications

Three-dimensional structure of mean motion resonances beyond Neptune

Three-dimensional structure of mean motion resonances beyond Neptune

Centaur and giant planet crossing populations: origin and distribution

“TNOs are Cool”: A survey of the trans-Neptunian region

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