Secular resonance sweeping and orbital excitation in decaying disks

Τόλιου, Αθανασία; Tsiganis, K.; Tsirvoulis, Georgios

doi:10.1007/s10569-019-9942-0

Cited by 10 publications

(3 citation statements)

References 40 publications

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“…Its efficiency in rising their inclinations mainly depends on the angle between the planetary and the MD planes. While revising this manuscript we became aware of the work of Toliou and Tsiganis (2019), performed independently, that find results similar to ours on the existence and the role of a non-zero f 5 frequency during the disk phase.…”

Section: Resultssupporting

confidence: 54%

Positions of the secular resonances in the primordial Kuiper Belt disk

Baguet

Morbidelli

Petit

2019

Icarus

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The dynamically hot and cold populations of the Kuiper Belt probably formed from two distinct regions of the Solar System. The former originated from a massive planetesimal disk extending from the primordial position of Neptune to ∼30 AU and the latter from a light extension of the planetesimal disk, prolonging beyond 30 AU. Previous studies on the dynamical evolution of the primordial cold population only accounted for the giant planets and did not consider its evolution under the influence of the massive part of the planetesimal disk. The latter affects it only indirectly through its interactions with the giant planets. Our goal is to introduce the perturbation of the massive part of the planetesimal disk on the apsidal and nodal precessions of both the giant planets and planetesimals, using the linear secular theory. We want to see how it affects the positions of the secular resonances. In the first place, we look at the positions of the secular resonances after the disappearance of the solar nebula, when the giant planets were locked in a multiresonant configuration. Because of this multiresonant configuration, the linear secular theory allows us to compute only the nodal part. The existence of a massive disk of planetesimals makes the f 5 frequency non-zero. We show that the associated secular resonance is located in the region corresponding to the current cold Kuiper Belt in several multiresonant configurations of the giant planets. The efficiency of this secular resonance in rising the inclinations of the objects depends on the misalignment between the total angular momentum of the giant planets and the direction orthogonal to the massive planetesimal disk. If both are aligned, the amplitude associated to the f 5 frequency is null and the resonance has no effect. We illustrate this

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Section: Resultssupporting

confidence: 54%

Positions of the secular resonances in the primordial Kuiper Belt disk

Baguet

Morbidelli

Petit

2019

Icarus

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“…The mechanism that we invoke to transport planetesimals inward is based on the sweeping of secular resonances to drive eccentricity excitation and gas drag to damp them, causing orbital decay. The sweeping arises from the commensurability between the apsidal precession rates of the Jovian planet and that of the planetesimals (Heppenheimer 1980;Ward 1981), a process that has been studied in various contexts, including the dynamics of asteroids in the Solar System (Lemaitre & Dubru 1991;Nagasawa et al 2000;Zheng et al 2017aZheng et al , 2017bGong et al 2019) and the excitation of planetary eccentricities and/or inclinations (Hahn & Malhotra 1999;Nagasawa et al 2003;Petrovich et al 2019;Toliou et al 2019).…”

Section: Sweeping Secular Resonancesmentioning

confidence: 99%

The Influence of Cold Jupiters in the Formation of Close-in Planets. I. Planetesimal Transport

Best,

Sefilian,

Petrovich

2023

ApJ

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The formation of a cold Jupiter (CJ) is expected to quench the influx of pebbles and the migration of cores interior to its orbit, thus limiting the efficiency of rocky planet formation either by pebble accretion and/or orbital migration. Observations, however, show that the presence of outer CJs (>1 au and ≳0.3M Jup) correlates with the presence of inner super-Earths (at <1 au). This observation may simply be a result of an enhanced initial reservoir of solids in the nebula required to form a CJ or a yet-to-be-determined mechanism assisted by the presence of the CJ. In this work, we focus on the latter alternative and study the orbital transport of planetesimals interior to a slightly eccentric (∼0.05) CJ subject to the gravity and drag from a viscously evolving gaseous disk. We find that a secular resonance sweeping inward through the disk gradually transports rings of planetesimals when their drag-assisted orbital decay is faster than the speed of the resonance scanning. This snowplow-like process leads to large concentration (boosted by a factor of ∼10–100) of size-segregated planetesimal rings with aligned apsidal lines, making their expected collisions less destructive, due to their reduced velocity dispersion. This process is efficient for a wide range of α-disk models (and thus disk lifetimes) and Jovian masses, peaking for values ∼1–5M Jup, which are typical of observed CJs in radial velocity surveys. Overall, our work highlights the major role that the disk's gravity may have on the orbital redistribution of planetesimals, depicting a novel avenue by which CJs may enhance the formation of inner planetary systems, including super-Earths and perhaps even warm and hot Jupiters.

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“…The dynamics considered in the current section however might still be relevant for sub-Neptunes not capable of fully carving gaps. For more sophisticated models of disk evolution with planet-carved gaps we refer the reader to the recent work by Toliou et al (2019).…”

Section: Kepler-419: Planets Fully Embedded In a Photoevaporating Diskmentioning

confidence: 99%

Constraining protoplanetary disks with exoplanetary dynamics: Kepler-419 as an example

Ali-Dib,

Petrovich

2020

Preprint

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We investigate the origins of Kepler-419, a peculiar system hosting two nearly coplanar and highly eccentric gas giants with apsidal orientations librating around antialignment, and use this system to place constraints on the properties of their birth protoplanetary disk. We follow the proposal by Petrovich, Wu, & Ali-Dib (2019) that these planets have been placed on these orbits as a natural result of the precessional effects of a dissipating massive disk and extend it by using direct N-body simulations and models for the evolution of the gas disks, including photo-evaporation. Based on a parameter space exploration, we find that in order to reproduce the system the initial disk mass had to be at least 95 M Jup and dissipate on a timescale of at least 10 4 yr. This mass is consistent with the upper end of the observed disk masses distribution, and the dissipation timescale is consistent with photoevaporation models. We study the properties of such disks using simplified 1D thin disk models and show that they are gravitationally stable, indicating that the two planets must have formed via core accretion and thus prone to disk migration. We hence finally investigate the sensitivity of this mechanism to the outer planet's semi major axis, and find that the nearby 7:1, 8:1, and 9:1 mean-motion resonances can completely quench this mechanism, while even higher order resonances can also significantly affect the system. Assuming the two planets avoid these high order resonances and/or close encounters, the dynamics seems to be rather insensitive to planet c semi major axis, and thus orbital migration driven by the disk.

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Secular resonance sweeping and orbital excitation in decaying disks

Cited by 10 publications

References 40 publications

Positions of the secular resonances in the primordial Kuiper Belt disk

Positions of the secular resonances in the primordial Kuiper Belt disk

The Influence of Cold Jupiters in the Formation of Close-in Planets. I. Planetesimal Transport

Constraining protoplanetary disks with exoplanetary dynamics: Kepler-419 as an example

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