Positions of the secular resonances in the primordial Kuiper Belt disk

Baguet, Daniel; Morbidelli, Alessandro; Petit, Jean-Marc

doi:10.1016/j.icarus.2019.113417

Cited by 6 publications

(5 citation statements)

References 33 publications

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“…As can be easily seen on this plot, the s 5 secular frequency is not null, when the disk's mass is non-zero and, hence, it can be very important for the secular dynamics of asteroids during that period. The possible importance of the s 5 resonance was also recently noted by Baguet et al (2019), in their study of the effect of a massive planetesimal disk on the dynamics of primordial Kuiper Belt Objects (KBOs). The presence of the disk has an effect similar to that of an oblate central body, i.e.…”

Section: Numerical Representation Of a Diskmentioning

confidence: 63%

Secular resonance sweeping and orbital excitation in decaying disks

Τόλιου¹,

Tsiganis²,

Tsirvoulis³

2019

Celest Mech Dyn Astr

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We revisit the problem of secular resonance sweeping during the dissipation of a protoplanetary disk and its possible role in exciting the orbits of primordial asteroids, in the light of recent models of solar system evolution. We develop an integrator that incorporates the gravitational effect of a uniformly (or not) depleting, axisymmetric disk with arbitrary surface density profile; its performance is verified by analytical calculations. The secular response of fictitious asteroids, under perturbations from Jupiter, Saturn and a decaying disk, is thoroughly studied. Note that the existence of a symmetry plane induced by the disk, lifts the inherent degeneracy of the two-planet system, such that the "s 5 " nodal frequency can also play a major role. We examine different resonant configurations for the planets (2:1, 3:2, 5:3), disk models and depletion scenarios. For every case we compute the corresponding time paths of secular resonances, which show when and where resonance crossing occurs. The excitation of asteroids, particularly in inclination, is studied in the various models and compared to analytical estimates. We find that inclination excitation in excess of ∼ 10 • is possible in the asteroid belt, but the nearly uniform spread of ∆i ∼ 20 • observed calls for the combined action of secular resonance sweeping with other mechanisms (e.g. scattering by Mars-sized embryos) that would be operating during terrestrial planet formation. Our results are also applicable to extrasolar planetary systems.

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Section: Numerical Representation Of a Diskmentioning

confidence: 63%

Secular resonance sweeping and orbital excitation in decaying disks

Τόλιου¹,

Tsiganis²,

Tsirvoulis³

2019

Celest Mech Dyn Astr

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“…The absence of low-I TNOs here does not imply that the cold belt did not exist here before the giant planets finished formation and migration. How and when these secular resonances reached their current location is a subject of much speculation (egs., Batygin et al 2011, Dawson & Murray-Clay 2012, Gladman et al 2012, Nesvorný 2018, Baguet et al 2019 2. The double averaging method removes the apparent forced-inclination singularities that occur in the linear secular theory.…”

Section: Discussionmentioning

confidence: 99%

Free Inclinations for Transneptunian Objects in the Main Kuiper Belt

Huang,

Gladman,

Volk

2022

Preprint

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There is a complex inclination structure present in the transneptunian object (TNO) orbital distribution in the main classical belt region (between orbital semimajor axes of 39 and 48 au). The long-term gravitational effects of the giant planets make TNO orbits precess, but non-resonant objects maintain a nearly constant 'free' inclination (I free ) with respect to a local forced precession pole. Because of the likely cosmogonic importance of the distribution of this quantity, we tabulate free inclinations for all main-belt TNOs, each individually computed using barycentric orbital elements with respect to each object's local forcing pole. We show that the simplest method, based on the Laplace-Lagrange secular theory, is unable to give correct forcing poles for objects near the ν 18 secular resonance, resulting in poorly conserved I free values in much of the main belt. We thus instead implemented an averaged Hamiltonian to obtain the expected nodal precession for each TNO, yielding significantly more accurate free inclinations for non-resonant objects. For the vast majority (96%) of classical belt TNOs, these I free values are conserved to < 1 • over 4 Gyr numerical simulations, demonstrating the advantage of using this well-conserved quantity in studies of the TNO population and its primordial inclination profile; our computed distributions only reinforce the idea of a very co-planar surviving 'cold' primordial population, overlain by a large I-width implanted 'hot' population.

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“…We selected the simulations that best satisfy the criteria of similarity with the Solar System today, consistent with the current orbital structure of the trans-Neptunian population, in line with Deienno et al (2017), which were all from the 3:2, 3:2, 2:1, 3:2 multi-resonance configuration, with a disk of 40 M C . The initial multi-resonant configurations we choose for Jupiter, Saturn, Uranus, Neptune, and I1, along with parameters for the location and mass of disk, begin in a 3:2, 3:2, 2:1, 3:2 resonance, as Baguet et al (2019) find this is able to place a secular tilt resonance in the area of the cold Edgeworth-Kuiper belt (between 39 and 48 au). This provides us with five scenarios to explore, as defined in Table 1.…”

Section: Methodsmentioning

confidence: 99%

Volatile-rich comets ejected early on during Solar System formation

Anderson

Petit

Noyelles

et al. 2022

A&A

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Context. Comet C/2016 R2 PanSTARRS (hereafter C/2016 R2) presents an unusually high N 2 /CO abundance ratio, as well as a heavy depletion in H 2 O, making it the only known comet of its kind. Understanding its dynamical history is therefore of essential importance as it would allow us to gain a clearer understanding of the evolution of planetesimal formation in our Solar System. Two studies have independently estimated the possible origin of this comet from building blocks formed in a peculiar region of the protoplanetary disk, near the ice line of CO and N 2 . Aims. We intend to investigate the fates of objects formed from the building blocks in these regions. We hope to find a possible explanation for the lack of C/2016 R2-like comets in our Solar System. Methods. Using a numerical simulation of the early stages of Solar System formation, we track the dynamics of these objects in the Jumping Neptune scenario based on five different initial conditions for the protosolar disk. We integrate the positions of 250 000 planetesimals over time in order to analyze the evolution of their orbits and create a statistical profile of their expected permanent orbit.Results. We find that objects formed in the region of the CO-and N 2 -ice lines are highly likely to be sent towards the Oort Cloud or possibly ejected from the Solar System altogether on a relatively short timescale. In all our simulations, over 90% of clones formed in this region evolved into a hyperbolic trajectory, and between 1% and 10% were potentially captured by the Oort Cloud. The handful of comets that remained were either on long-period, highly eccentric orbits like C/2016 R2, or absorbed into the Edgeworth-Kuiper belt. Conclusions. Comets formed <15 au were predominantly ejected early in the formation timeline. As this is the formation zone likely to produce comets of this composition, this process could explain the lack of similar comets observed in the Solar System.

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Positions of the secular resonances in the primordial Kuiper Belt disk

Cited by 6 publications

References 33 publications

Secular resonance sweeping and orbital excitation in decaying disks

Secular resonance sweeping and orbital excitation in decaying disks

Free Inclinations for Transneptunian Objects in the Main Kuiper Belt

Volatile-rich comets ejected early on during Solar System formation

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