CHAOTIC DIFFUSION OF RESONANT KUIPER BELT OBJECTS

@article{Tiscareno2004CHAOTICDO,
  title={CHAOTIC DIFFUSION OF RESONANT KUIPER BELT OBJECTS},
  author={Matthew S. Tiscareno and Renu Malhotra},
  journal={The Astronomical Journal},
  year={2004},
  volume={138},
  pages={827 - 837}
}
We carried out extensive numerical orbit integrations to probe the long-term chaotic dynamics of the two strongest mean-motion resonances of Neptune in the Kuiper Belt, the 3:2 (Plutinos) and 2:1 (Twotinos). Our primary results include a computation of the relative volumes of phase space characterized by large- and small-resonance libration amplitudes, and maps of resonance stability measured by mean chaotic diffusion rate. We find that Neptune's 2:1 resonance has weaker overall long-term… 

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TLDR
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References

SHOWING 1-10 OF 46 REFERENCES

Chaotic Diffusion and the Origin of Comets from the 2/3 Resonance in the Kuiper Belt

Abstract The dynamical structure of the 2/3 resonance at small inclination is explored using numerical integrations of test particles to compute the evolution of proper elements with time. The basic

Mean Motion Resonances in the Trans-neptunian Region

The stability of the 2:3 mean motion resonance with Neptune is systematically explored and compared to the observed resonant population. It is shown that orbits with small and moderate amplitudes of

On the Plutinos and Twotinos of the Kuiper Belt

We illuminate dynamical properties of Kuiper belt objects (KBOs) in the 3 : 2 (Plutino) and 2 : 1 ("Twotino") Neptunian resonances within the model of resonant capture and migration. We analyze a

Mean Motion Resonances in the Transneptunian Region. Part II: The 1 : 2, 3 : 4, and Weaker Resonances

Abstract The stability of orbits in the transneptunian region is numerically computed. It is found that, in analogy to the asteroid belt, there exist many chaotic layers associated with thin

The Phase Space Structure Near Neptune Resonances in the Kuiper Belt

The Solar system beyond Neptune is believed to house a population of small primordial bodies left over from the planet formation process. The region up to heliocentric distance -50 AU (a.k.a. the

The Dynamics of Known Centaurs

We have numerically investigated the long-term dynamical behavior of known Centaurs. This class of objects is thought to constitute the transitional population between the Kuiper belt and the

Close Approaches of Trans-Neptunian Objects to Pluto Have Left Observable Signatures on Their Orbital Distribution

It is shown that in addition to four outer planets (Jupiter to Neptune) Pluto should be also taken into account in studies of the orbital dynamics in the trans-Neptunian region. Pluto's effect is

Simulations of the population of Centaurs – I. The bulk statistics

Large-scale simulations of the Centaur population are carried out. The evolution of 23 328 particles based on the orbits of 32 well-known Centaurs is followed for up to 3 Myr in the forward and

From the Kuiper Belt to Jupiter-Family Comets: The Spatial Distribution of Ecliptic Comets☆

Abstract We present numerical orbital integrations of thousands of massless particles as they evolve from Neptune-encountering orbits in the Kuiper belt for up to 1 Gyr or until they either impact a