Journal Article10.1006/ICAR.1999.6147
Dynamical Evolution of Planetesimals in the Outer Solar System II. The Saturn/Uranus and Uranus/Neptune Zones
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TL;DR: In this article, the authors reported on numerical simulations exploring the dynamical stability of planetesimals in the gaps between the outer Solar System planets, using high-order optimized multistep integration schemes coupled with roundoff error minimizing methods.
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About: This article is published in Icarus. The article was published on 01 Aug 1999. The article focuses on the topics: Planetary migration & Uranus.
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Citations
GLISSE: A GPU-optimized planetary system integrator with application to orbital stability calculations.
TL;DR: It is explained how various hardware speed bottlenecks can be avoided by the careful code design, although some of the choices restrict the usage to specific types of application.
Dynamical delivery of volatiles to the outer main belt
TL;DR: In this article, the authors quantify the relative contribution of volatiles supplied from outer Solar System planetesimal reservoirs to large wet asteroids during the first few My after the beginning of the Solar System.
The dynamics of known centaurs
TL;DR: In this paper, the authors investigated the long-term dynamical behavior of known Centaurs and found that over their dynamical lifetimes these objects diffuse into the JFCs and other sinks, and they also make excursions into the scattered disk, but do not diffuse into a parameter space representing the main Kuiper belt.
The resonant dynamical evolution of small body orbits among giant planets
TL;DR: In this paper, the authors show that even in one of the most chaotic regions of the Solar System, the region of the giant planets, there are numerous bands where mean motion resonances can stabilize orbits of small bodies in a time span comparable to their lifetimes.
Stochasticity and predictability in terrestrial planet formation
TL;DR: In this article, the authors use numerical simulations to show that practically identical initial conditions result in a wide array of final planetary configurations, which is a result of the chaotic evolution of trajectories which are highly sensitive to minuscule displacements.
References
Symplectic maps for the N-body problem.
Jack Wisdom,Matthew J. Holman +1 more
TL;DR: In this paper, the authors generalize the mapping method of Wisdom (1982) to encompass all gravitational n-body problems with a dominant central mass and use it to compute the evolution of the outer planets for a billion years.
1.3K
Some dynamical aspects of the accretion of Uranus and Neptune: The exchange of orbital angular momentum with planetesimals
J.A. Fernández,Wing-Huen Ip +1 more
TL;DR: In this paper, the final stage of the accretion of Uranus and Neptune is numerically investigated and two possible effects that may have contributed to the formation of the two outer Jovian planets are incorporated in the model.
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The origin of Pluto's peculiar orbit
TL;DR: The origin of Pluto's unusual orbit is still a mystery as mentioned in this paper, and the most eccentric and inclined of all the planets still remains a mystery, although it has been shown that Pluto could have acquired its current orbit during the late stages of planetary accretion when the jovian planets underwent significant orbital migration as a result of encounters with residual planetesimals.
501
The Origin of Pluto's Peculiar Orbit
Renu Malhotra
- 01 Mar 1995
TL;DR: The origin of Pluto's unusual orbit is still a mystery as mentioned in this paper, and the most eccentric and inclined of all the planets still remains a mystery, although it has been shown that Pluto could have acquired its current orbit during the late stages of planetary accretion when the jovian planets underwent significant orbital migration as a result of encounters with residual planetesimals.
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