The origin of Pluto's peculiar orbit

Malhotra, Renu

doi:10.1038/365819a0

Cited by 441 publications

(399 citation statements)

References 14 publications

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“…Outward migration is possible if a significant fraction of the perturbed planetesimals collide with the central star (or, in the case of multiple planets, if planetesimals are passed inward from planet to planet until an ejection occurs; cf. Malhotra 1993). Due to the large number of particles required to simulate this process and the long timescales involved, this problem has been out of reach of direct methods.…”

Section: Model D: Orbital Migrationmentioning

confidence: 99%

“…One type of orbital migration that may be amenable to direct simulation arises from planetestimal scattering (Malhotra 1993, Murray et al 1998. In this scenario, planetesimals lose angular momentum through resonant interactions with a planet embedded in the disk.…”

Section: Model D: Orbital Migrationmentioning

confidence: 99%

“…Recent discoveries (e.g., Marcy et al 1998 and references therein) of giant planets in surprisingly small orbits around nearby stars have stimulated an interest in orbital migration (Lin et al 1996) that may arise from gravitational torques (Goldreich and Tremaine 1980), excitation of spiral density waves in the gaseous disk (Ward 1986(Ward , 1997, or preferential scattering of planetesimals (Malhotra 1993, Murray et al 1998. Jupiter could also drive a one-armed spiral density wave in the planetesimal disk of wavelength ∼0.5 AU (for nominal disk parameters) at the g5 secular resonance near 2 AU, creating a spiral wave pattern that rotates on a timescale of ∼10 5 yr (Ward and Hahn 1998).…”

Section: Outstanding Issues In Planet Formationmentioning

confidence: 99%

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Direct Large-Scale N-Body Simulations of Planetesimal Dynamics

Richardson

Quinn

Stadel

et al. 2000

Icarus

229

210

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We describe a new direct numerical method for simulating planetesimal dynamics in which N ∼ 10 6 or more bodies can be evolved simultaneously in three spatial dimensions over hundreds of dynamical times. This represents several orders of magnitude improvement in resolution over previous studies. The advance is made possible through modification of a stable and tested cosmological code optimized for massively parallel computers. However, owing to the excellent scalability and portability of the code, modest clusters of workstations can treat problems with N ∼ 10 5 particles in a practical fashion.The code features algorithms for detection and resolution of collisions and takes into account the strong central force field and flattened Keplerian disk geometry of planetesimal systems. We demonstrate the range of problems that can be addressed by presenting simulations that illustrate oligarchic growth of protoplanets, planet formation in the presence of giant planet perturbations, the formation of the jovian moons, and orbital migration via planetesimal scattering. We also describe methods under development for increasing the timescale of the simulations by several orders of magnitude.

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Section: Model D: Orbital Migrationmentioning

confidence: 99%

Section: Model D: Orbital Migrationmentioning

confidence: 99%

Section: Outstanding Issues In Planet Formationmentioning

confidence: 99%

See 1 more Smart Citation

Direct Large-Scale N-Body Simulations of Planetesimal Dynamics

Richardson

Quinn

Stadel

et al. 2000

Icarus

229

210

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“…Migration due to interactions between planets and planetesimal disk is well studied in the evolution of outer solar system (e.g., Malhotra 1993, Hahn & Malhotra, 1999. The direction of the planet migrations is mainly determined by the averaged angular momentum H = a(1 − e 2 ) of the planetesimals.…”

Section: Interactions Between Planets and Planetesimal Diskmentioning

confidence: 99%

Dynamical evolution of extrasolar planetary systems

Zhou

Sun

2004

Proc. IAU

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Abstract. To date, more than 130 extrasolar planets around main sequence stars are revealed mainly by the Doppler radial velocity measurements. Due to the observational biases, most of the detected planets are moving in orbits close to the host stars, with some in highly eccentric orbits. Dynamical processes during the late stage of planet formation are important to account for the present orbital properties. These processes include: planet migrations and resonance trappings caused by gravitational interactions between protostellar disk and planets, dynamical scattering due to interactions between planets, etc. In this paper, we review the major effects of these dynamical processes on the orbital characteristics of the planet systems.

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“…However, Morbidelli (1997) studied a uniform distribution of initial orbits. Now we know that the mechanism of Neptune's migration is very important in the formation of the resonant population structure (Malhotra 1993(Malhotra , 1995Hahn & Malhotra 1999.…”

Section: Introductionmentioning

confidence: 99%

Resonant trans-Neptunian objects as a source of Jupiter-family comets

Kiseleva¹,

Emel’yanenko²

2006

Proc. IAU

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Abstract. The dynamical interrelation between resonant trans-Neptunian objects and shortperiod comets is studied. Initial orbits of resonant objects are based on computations in the model of the outward transport of objects during Neptune's migration in the early history of the outer Solar system. The dynamical evolution of this population is investigated for 4.5 Gyr, using a symplectic integrator. Our calculations show that resonant trans-Neptunian objects give a substantial contribution to the planetary region. We have estimated that the relative fraction of objects captured per year from the 2/3 resonance to Jupiter-family orbits with perihelion distances q < 2.5 AU is 0.4 × 10 −10 near the present epoch.

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The origin of Pluto's peculiar orbit

Cited by 441 publications

References 14 publications

Direct Large-Scale N-Body Simulations of Planetesimal Dynamics

Direct Large-Scale N-Body Simulations of Planetesimal Dynamics

Dynamical evolution of extrasolar planetary systems

Resonant trans-Neptunian objects as a source of Jupiter-family comets

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