High-eccentricity trans-Neptunian objects as a source of Jupiter-family comets

Emel’yanenko, V. V.; Asher, D. J.; Bailey, Mark

doi:10.1111/j.1365-2966.2004.07624.x

Cited by 30 publications

(42 citation statements)

References 26 publications

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“…These have been shown to provide a small flux of material into Neptune's chaotic zone in our solar system (e.g. Duncan et al 1995;Holman & Wisdom 1993;Levison & Duncan 1997;Emel'yanenko et al 2004;Morbidelli 1997). This contribution cannot be significant as in our simulations to test this effect with a particle density of 50 particles per AU, not a single particle, that started outside of a max = a pl +2δa chaos and inside of 100 AU, was scattered inwards, although there was evidence of the effect of the inner planets on the outer regions of the belt.…”

Section: Uncertaintiesmentioning

confidence: 99%

Scattering of small bodies by planets: a potential origin for exozodiacal dust?

Bonsor

Augereau

Thébault

2012

A&A

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High levels of exozodiacal dust are observed around a growing number of main sequence stars. The origin of such dust is not clear, given that it has a short lifetime against both collisions and radiative forces. Even a collisional cascade with km-sized parent bodies, as suggested to explain outer debris discs, cannot survive sufficiently long. In this work we investigate whether the observed exozodiacal dust could originate from an outer planetesimal belt. We investigate the scattering processes in stable planetary systems to determine whether sufficient material could be scattered inwards in order to retain the exozodiacal dust at its currently observed levels. We use N-body simulations to investigate the efficiency of this scattering and its dependence on the architecture of the planetary system. The results of these simulations can be used to assess the ability of hypothetical chains of planets to produce exozodi in observed systems. We find that for older (>100 Myr) stars with exozodiacal dust, a massive, large radii (>20 AU) outer belt and a chain of tightly packed, low-mass planets would be required to retain the dust at its currently observed levels. This brings into question how many, if any, real systems possess such a contrived architecture and are therefore capable of scattering at sufficiently high rates to retain exozodi dust on long timescales.

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Section: Uncertaintiesmentioning

confidence: 99%

Scattering of small bodies by planets: a potential origin for exozodiacal dust?

Bonsor

Augereau

Thébault

2012

A&A

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“…Since the JFCs originate in scattered disc Emel'yanenko et al 2004;Volk & Malhotra 2008;Di Sisto et al 2009;Brasser & Morbidelli 2013), we also update the inferred number of scattered disc objects (SDOs) by using the total number of active JFCs as a proxy. To compare our simulation with the observational data we need to have an observational catalogue of comets that is as complete as possible.…”

Section: Observational Datasetmentioning

confidence: 99%

An updated estimate of the number of Jupiter-family comets using a simple fading law

Brasser

Wang

2015

A&A

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It has long been hypothesised that the Jupiter-family comets (JFCs) come from the scattered disc, an unstable planetesimal population beyond Neptune. This viewpoint has been widely accepted, but a few issues remain, the most prominent of which are the total number of visible JFCs with a perihelion distance q < 2.5 AU and the corresponding number of objects in the scattered disc. In this work we give a robust estimate of the number of visible JFCs with q < 2.5 AU and diameter D > 2.3 km based on recent observational data. This is combined with numerical simulations that use a simple fading law applied to JFCs that come close to the Sun. For this we numerically evolve thousands of comets from the scattered disc through the realm of the giant planets and keep track of their number of perihelion passages with perihelion distance q < 2.5 AU, below which the activity is supposed to increase considerably. We can simultaneously fit the JFC inclination and semi-major axis distribution accurately with a delayed power law fading function of the form Φ m ∝ (M 2 + m 2 ) −k/2 , where Φ m is the visibility, m is the number of perihelion passages with q < 2.5 AU, M is an integer constant, and k is the fading index. We best match both the inclination and semi-major axis distributions when k ∼ 1.4, M = 40, and the maximum perihelion distance below which the observational data is complete is q m ∼ 2.3 AU. From observational data we calculate that a JFC with diameter D = 2.3 km has a typical total absolute magnitude H T = 10.8, and the steady-state number of active JFCs with diameter D > 2.3 km and q < 2.5 AU is of the order of 300 (but with large uncertainties), approximately a factor two higher than earlier estimates. The increased JFC population results in a scattered disc population of 6 billion objects and decreases the observed Oort cloud to scattered disc population ratio to 13, virtually the same as the value of 12 obtained with numerical simulations.

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“…This distribution is consistent with the observed distribution of Jupiter-family comets. However, this distribution is more concentrated towards high values of Tisserand parameter than that in models studying high-eccentricity trans-Neptunian objects (Emel'yanenko et al 2004) and objects from the Oort cloud (Emel'yanenko et al 2005) as sources of Jupiter-family comets. …”

Section: Evolution To Jupiter-family Orbitsmentioning

confidence: 71%

“…We study the orbital evolution of these objects until they are captured to q < 2.5 au or evolve to a hyperbolic orbit. We then apply the method described in Emel'yanenko et al (2004) to calculate the rate of injection of Jupiter-family comets from the 2/3 resonant population.…”

Section: Evolution For the Age Of The Solar Systemmentioning

confidence: 99%

“…It was shown by Duncan & Levison (1997) and by Emel'yanenko et al (2004) that the scattered disc trans-Neptunian objects are a source of Jupiter-family comets. On the other hand, Morbidelli (1997), and Nesvorný & Roig (2000) demonstrated that objects from the classical Edgeworth-Kuiper belt moving in the resonance 2/3 with Neptune can also contribute to the population of Jupiter-family comets.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

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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High-eccentricity trans-Neptunian objects as a source of Jupiter-family comets

Cited by 30 publications

References 26 publications

Scattering of small bodies by planets: a potential origin for exozodiacal dust?

Scattering of small bodies by planets: a potential origin for exozodiacal dust?

An updated estimate of the number of Jupiter-family comets using a simple fading law

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

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