Orbital Migration of Neptune and Orbital Distribution of Trans‐Neptunian Objects
Open accessAbstract
A large number of trans-Neptunian objects are found to have orbits that are commensurate with the 3 : 2 mean-motion resonance of Neptune's orbit. These objects were probably captured into this resonant configuration when proto-Neptune migrated outward from its cradle. Up to now, only a few objects have been found at Neptune's 2 : 1 resonance (which is also a strong mean-motion resonance). This observed distribution of objects provides a strong constraint on the migration timescale and mechanism. With a series of numerical simulations, we show that Neptune would indeed trap objects onto its 3 : 2 resonance if it were to migrate outward over a timescale ≳10 6 yr. But in order to avoid the concurrent capture of objects onto its 2 : 1 resonance, Neptune's migration timescale must be ≲10 7 yr. Thus, the resonant capture process is likely to have occurred during the epoch of protoplanetary formation. We examine two potential mechanisms that are both compatible with the constraint set by the orbital distribution of trans-Neptunian objects. (1) In the cold outer regions of the gaseous solar nebula, proto-Neptune's tidal perturbation may have led to the formation of a gap near its orbit, the termination of its gas accretion, and the migration of its orbit along with the viscous expansion of the solar nebula on the timescale of ~10 6 -10 7 yr. This scenario is appealing because it can also naturally account for the limited amount of gas in Neptune's envelope. For self-consistency, we show that it is possible for proto-Neptune to acquire its core and envelope mass within the characteristic persistence timescale of protostellar disks (~10 6 -10 7 yr) with an inferred solid material/gas surface density comparable to/less than those of the minimum-mass nebula, respectively. (2) During its initial buildup, proto-Neptune's core not only collided and coagulated with residual planetesimals but also underwent close scatterings with large-angle deflection. We demonstrate with numerical simulations that such a process may lead to the expansion of its orbit over a few 10 6 yr. The asymmetrical planetesimal distribution that drives this migration is self-sustained by the planetesimal scatterings and the migration. In other words, the migration occurs without help of other giant planets, unlike the migration models of other authors (e.g., Fernandez & Ip; Hahn & Malhotra) which rely on planetesimal depletion due to ejection by the strong gravitational effects of proto-Jupiter and proto-Saturn. The main advantages of this alternative scenario are that (1) it provides a fresh replenishment of residual planetesimals into the feeding zone such that proto-Neptune may acquire a core more massive than the isolation mass within ~10 7 yr and (2) resonant trapping may lead to a natural termination of both proto-Neptune's planetesimal accretion and its orbital migration, determining its present core mass and position in a self-consistent manner.
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Analytic and numerical calculations show that isolated planets migrate through the disk on a timescale much shorter than the disk lifetime.
“Analytic and numerical calculations show that, in many cases, isolated planets migrate through the disk on a timescale much shorter than the disk lifetime”
From MIGRATION OF SMALL MOONS IN SATURN's RINGS (2013) · cites this paper as Ida et al. 2000
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- Authors
- Ida, S., Bryden, G., Lin, D. N. C., & Tanaka, H.
- Affiliations
- Tokyo Institute of Technology (JP)
- University of California, Santa Cruz (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2000-05
- Volume
- 534
- Issue
- 1
- Pages
- 428-445
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2076469174
- Cited by
- 152
- References
- 62
- Citations by year
- 2026: 5 · 2025: 5 · 2024: 2 · 2023: 4 · 2022: 4 · 2021: 2 · 2020: 17 · 2019: 3 · 2018: 5 · 2017: 2 · 2016: 4 · 2015: 5 · 2014: 6 · 2013: 5 · 2012: 9
- FWCI
- 6.18
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- Tokyo Tech Research Repository (Tokyo Institute of Technology) (submittedVersion)
- Funders
- National Science Foundation (9618548, 9714275)
- National Aeronautics and Space Administration (NAG57515)
- University of California, Santa Cruz
- Ames Research Center
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysics and Star Formation Studies
- Keywords
- trans-Neptunian objects, mean motion resonance, 3:2 resonance, 2:1 resonance, resonance capture, protoplanetary disks, tidal perturbations, gas accretion, planetesimal scattering, giant planet formation, planetesimal disk, orbital distribution, solar nebula
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