Orbital and Collisional Evolution of the Irregular Satellites

Nesvorný, David; Alvarellos, J. L.; Dones, L.; Levison, Harold F.

doi:10.1086/375461

Cited by 189 publications

(326 citation statements)

References 65 publications

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“…The KL effect for ballistic objects has been applied to a wide range of astronomical processes. These range from inclinations of asteroids and irregular satellites (Kozai 1962;Nesvorný et al 2003) to tidal disruption events (Chen et al 2011), and the formation of Type Ia supernovae (Kushnir et al 2013).…”

Section: Introductionmentioning

confidence: 99%

Kozai–Lidov disc instability

Lubow

Ogilvie

2017

Monthly Notices of the Royal Astronomical Society

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Recent results by Martin et al. (2014) showed in 3D SPH simulations that tilted discs in binary systems can be unstable to the development of global, damped Kozai-Lidov (KL) oscillations in which the discs exchange tilt for eccentricity. We investigate the linear stability of KL modes for tilted inviscid discs under the approximations that the disc eccentricity is small and the disc remains flat. By using 1D equations, we are able to probe regimes of large ratios of outer to inner disc edge radii that are realistic for binary systems of hundreds of AU separations and are not easily probed by multidimensional simulations. For order unity binary mass ratios, KL instability is possible for a window of disc aspect ratios H/r in the outer parts of a disc that roughly scale as (n b /n) 2 < ∼ H/r < ∼ n b /n, for binary orbital frequency n b and orbital frequency n at the disc outer edge. We present a framework for understanding the zones of instability based on the determination of branches of marginally unstable modes. In general, multiple growing eccentric KL modes can be present in a disc. Coplanar apsidal-nodal precession resonances delineate instability branches. We determine the range of tilt angles for unstable modes as a function of disc aspect ratio. Unlike the KL instability for free particles that involves a critical (minimum) tilt angle, disc instability is possible for any nonzero tilt angle depending on the disc aspect ratio.

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Section: Introductionmentioning

confidence: 99%

Kozai–Lidov disc instability

Lubow

Ogilvie

2017

Monthly Notices of the Royal Astronomical Society

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“…Special care has been taken in the study of (i) the secular resonance ν =˙ −˙ (Saha & Tremaine 1993;Whipple & Shelus 1993;Beaugé & Nesvorný 2007;Nesvorný et al 2003;Yokoyama et al 2003;Ćuk & Burns 2004;Correa Otto et al 2009), which is one of the most important secular resonances acting on the satellites; (ii) the Lidov-Kozaï resonance for distant satellites (Beaugé et al 2006;Beaugé & Nesvorný 2007;Carruba et al 2002;Ćuk & Burns 2004;Nesvorný et al 2003); and (iii) the evection resonancė − n (Yokoyama et al 2008;Frouard et al 2010;Nesvorný et al 2003). In most of these works, the important need for the development of high-order perturbation methods or numerical ones is clearly stressed.…”

Section: Introductionmentioning

confidence: 99%

The long-term dynamics of the Jovian irregular satellites

Frouard

Vienne

Fouchard

2011

A&A

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Context. The dynamical region of the Jovian irregular satellites presents an interesting web of resonances that are not yet fully understood. Of particular interest is the influence of the resonances on the stochasticity of the individual orbits of the satellites, as well as on the long-term chaotic diffusion of the different families of satellites. Aims. We make a systematic numerical study of the satellite region to determine the important resonances for the dynamics, to search for the chaotic zones, and to determine their influences on the dynamics of the satellites. We also compare these numerical results to previous analytical works. Methods. Using extensive numerical integrations of the satellites along with an indicator of chaos (MEGNO), we show global and detailed views of the retrograde and prograde regions for various dynamical models of increasing complexity and indicate the appearance of the different types of resonances and the implied chaos. Results. Along with secular and mean motion resonances that shape the dynamical regions of the satellites, we report a number of resonances involving the Great Inequality, and which are present in the system thanks to the wide range of the values of frequencies of the pericenter available for the satellites. The chaotic diffusion of the satellites is also studied and shows the long-term stability of the Ananke and Carme families, in contrast to the Pasiphae family.

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“…The known irregular satellites are stable over the age of the Solar System though strongly influenced by solar and planetary perturbations (Henon 1970;Carruba et al 2002;Nesvorny et al 2003). The perturbations are most intense when the satellite is near 326 S. Sheppard apoapsis.…”

Section: Dynamics Of Irregular Satellitesmentioning

confidence: 99%

“…The perturbations are most intense when the satellite is near 326 S. Sheppard apoapsis. High inclination orbits have been found through numerical simulations to be unstable due to solar perturbations (Carruba et al 2002;Nesvorny et al 2003). Satellites with inclinations between 50 < i < 130 degrees slowly have their orbits stretched making them obtain very high eccentricities.…”

Section: Dynamics Of Irregular Satellitesmentioning

confidence: 99%

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Outer irregular satellites of the planets and their relationship with asteroids, comets and Kuiper Belt objects

Sheppard

2005

Proc. IAU

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Abstract. Outer satellites of the planets have distant, eccentric orbits that can be highly inclined or even retrograde relative to the equatorial planes of their planets. These irregular orbits cannot have formed by circumplanetary accretion and are likely products of early capture from heliocentric orbit. The irregular satellites may be the only small bodies remaining which are still relatively near their formation locations within the giant planet region. The study of the irregular satellites provides a unique window on processes operating in the young solar system and allows us to probe possible planet formation mechanisms and the composition of the solar nebula between the rocky objects in the main asteroid belt and the very volatile rich objects in the Kuiper Belt. The gas and ice giant planets all appear to have very similar irregular satellite systems irrespective of their mass or formation timescales and mechanisms. Water ice has been detected on some of the outer satellites of Saturn and Neptune whereas none has been observed on Jupiter's outer satellites.

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Orbital and Collisional Evolution of the Irregular Satellites

Cited by 189 publications

References 65 publications

Kozai–Lidov disc instability

Kozai–Lidov disc instability

The long-term dynamics of the Jovian irregular satellites

Outer irregular satellites of the planets and their relationship with asteroids, comets and Kuiper Belt objects

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