Evolution of Jovian planets in a self-gravitating planetesimal disk

Li, J.; Zhou, Li-Yong; Sun, Yi-Sui

doi:10.1051/0004-6361/201015601

Cited by 7 publications

(7 citation statements)

References 44 publications

(73 reference statements)

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“…The exponential behavior of outward migrations is successfully produced in these simulations. Recently Li et al (2011) improve this model by including the self-gravitation of the planetesimals and the similar results are obtained. For a model like this, it will be called as Gomes Migration hereafter in this paper.…”

Section: Introductionsupporting

confidence: 54%

“…Such a scenario was confirmed by Levison & Morbidelli (2003). However, it is not exactly known whether this "jumpy" migration, as apparently observed in the numerical simulations by Gomes (2004) and Li et al (2011), is a physically real behavior or it is just the artificial effects arising from the unrealistic large planetesimals applied in the simulations. In a theoretical model, the parameter such as the maximum radius of the scattering planetesimal, depends on the details of the disc status in the early stage of the Solar System.…”

Section: Introductionmentioning

confidence: 64%

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Modeling the Migration of Neptune and the Corresponding Resonant Captures

Yeh,

Jiang,

Zhou

2013

Preprint

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Due to the angular momentum exchange with planetesimals, Neptune might have migrated outward to the current position, and captured many Kuiper belt objects (KBOs) into resonances. We set up a semianalytic model to simulate the outward migration of Neptune, and the processes of resonant captures. Our model can naturally explain Neptune's currently observed semi-major axis and eccentricity. The results show that the current population ratio between 3:2 and 2:1 is mainly due to the original density distribution of KBOs, which might be related to drag-induced inward migrations of proto-KBOs.

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Section: Introductionsupporting

confidence: 54%

Section: Introductionmentioning

confidence: 64%

Modeling the Migration of Neptune and the Corresponding Resonant Captures

Yeh,

Jiang,

Zhou

2013

Preprint

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“…1, 10 Twotinos are in the leading resonance and only 4 are in the trailing resonance, such a number difference may support an even larger τ (Lykawka & Mukai 2007). Indeed, a time-scale of τ = 2 × 10 7 yr was derived by Li et al (2011) from N -body simulations for the orbital evolution of Jovian planets embedded in a self-gravitating planetesimal disc. This reasonable value has already been adopted in LZS14.…”

Section: Introductionmentioning

confidence: 97%

A study of the high-inclination population in the Kuiper belt – II. The Twotinos

Zhou

Sun

2014

Monthly Notices of the Royal Astronomical Society

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As the second part of our study, in this paper we proceed to explore the dynamics of the high-inclination Twotinos in the 1:2 Neptune mean motion resonance (NMMR). Depending on the inclination i, we show the existence of two critical eccentricities e a (i) and e c (i), which are lower limits of the eccentricity e for the resonant angle σ to exhibit libration and asymmetric libration, respectively. Accordingly, we have determined the libration centres σ 0 for inclined orbits, which are strongly dependent on i. With initial σ = σ 0 on a fine grid of (e, i), the stability of orbits in the 1:2 NMMR is probed by 4-Gyr integrations. It is shown that symmetric librators are totally unstable for i 30 • ; while stable asymmetric librators exist for i up to 90 • .We further investigate the 1:2 NMMR capture and retention of planetesimals with initial inclinations i 0 90 • in the planet migration model using a time-scale of 2 × 10 7 yr. We find that: (1) the capture efficiency of the 1:2 NMMR decreases drastically with the increase of i 0 , and it goes to 0 when i 0 60 • ; (2) the probability of discovering Twotinos with i > 25 • , beyond observed values, is roughly estimated to be 0.1 per cent; (3) more particles are captured into the leading rather than the trailing asymmetric resonance for i 0 10 • , but this number difference appears to be the opposite at i 0 = 20 • and is continuously varying for even larger i 0 ; (4) captured Twotinos residing in the trailing resonance or having i > 15 • are practically outside the Kozai mechanism, like currently observed samples.

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“…The simulations on which we report do not take into account the role that jovian planetary migration may have had on the evolution of particles in the inter-planet gaps. There is no universal agreement upon the distance that the jovian planets migrated, or even the direction-with some results suggesting the jovians migrated inward (Franklin et al, 2004;Li et al, 2011), some outward (Gomes et al, 2005), some both (Walsh et al, 2011). Some of the results of these recent studies are mutually exclusive.…”

Section: Integration Methods and Initial Conditionsmentioning

confidence: 90%

Jupiter: Cosmic Jekyll and Hyde

Grazier

2016

Astrobiology

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It has been widely reported that Jupiter has a profound role in shielding the terrestrial planets from comet impacts in the Solar System, and that a jovian planet is a requirement for the evolution of life on Earth. To evaluate whether jovians, in fact, shield habitable planets from impacts (a phenomenon often referred to as the "Jupiter as shield" concept), this study simulated the evolution of 10,000 particles in each of the jovian inter-planet gaps for the cases of full-mass and embryo planets for up to 100 My. The results of these simulations predict a number of phenomena that not only discount the "Jupiter as shield" concept, they also predict that in a Solar System like ours, large gas giants like Saturn and Jupiter had a different, and potentially even more important, role in the evolution of life on our planet by delivering the volatile-laden material required for the formation of life. The simulations illustrate that, although all particles occupied "non-life threatening" orbits at their onset of the simulations, a significant fraction of the 30,000 particles evolved into Earth-crossing orbits. A comparison of multiple runs with different planetary configurations revealed that Jupiter was responsible for the vast majority of the encounters that "kicked" outer planet material into the terrestrial planet region, and that Saturn assisted in the process far more than has previously been acknowledged. Jupiter also tends to "fix" the aphelion of planetesimals at its orbit irrespective of their initial starting zones, which has the effect of slowing their passages through the inner Solar System, and thus potentially improving the odds of accretion of cometary material by terrestrial planets. As expected, the simulations indicate that the full-mass planets perturb many objects into the deep outer Solar System, or eject them entirely; however, planetary embryos also did this with surprising efficiency. Finally, the simulations predict that Jupiter's capacity to shield or intercept Earth-bound comets originating in the outer Solar System is poor, and that the importance of jovian planets on the formation of life is not that they act as shields, but rather that they deliver life-enabling volatiles to the terrestrial planets.

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Evolution of Jovian planets in a self-gravitating planetesimal disk

Cited by 7 publications

References 44 publications

Modeling the Migration of Neptune and the Corresponding Resonant Captures

Modeling the Migration of Neptune and the Corresponding Resonant Captures

A study of the high-inclination population in the Kuiper belt – II. The Twotinos

Jupiter: Cosmic Jekyll and Hyde

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