Analysing the region of the rings and small satellites of Neptune

Gallardo, D. M. Gaslac; Winter, S. M. Giuliatti; Madeira, Gustavo; Muñoz-Gutiérrez, Marco A.

doi:10.1007/s10509-019-3717-7

Cited by 5 publications

(2 citation statements)

References 26 publications

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“…The former were assumed by us as the building blocks of the moonlets, while the latter may have contributed to the formation of the arcs. As shown in Gallardo et al ( 2020 ), the dust material in the Adams ring region has a short lifetime due to solar radiation and plasma drag, so macroscopic debris are the most likely to have contributed to the formation of the arcs.…”

Section: Moon Disruption Stagementioning

confidence: 99%

“…We emphasize that the type of impactor influences the sizes of the launched particles. The impacts of IDPs produce micrometre particles (1-100 μm) that suffer the effects of dissipative forces, such as the solar radiation force and plasma drag (see Gallardo et al 2020 ). Giuliatti showed that the lifetime of micrometre particles in the arcs under the effects of the solar radiation force is less than 50 yr and that moonlets cannot replenish the arcs by IDP impacts.…”

Section: Post-formation Stagementioning

confidence: 99%

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Numerical analysis of processes for the formation of moonlets confining the arcs of Neptune

Madeira

Winter

2022

Monthly Notices of the Royal Astronomical Society

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The arcs of Neptune - FraternitÃ©, EgalitÃ©, LibertÃ©, and Courage - are four incomplete rings immersed in the Adams ring. A recent confinement model for the arcs proposes that the structures are azimuthally confined by four co-orbital moonlets. In this work, we intend to approach some points related to the dynamics of co-orbital moonlets and suggest a model for their formation. We study the equilibrium configurations for 1+N co-orbital satellites under the 42:43 Lindblad resonance with Galatea. We obtained three distinct configurations with 1+3 and 1+4 moonlets able to confine and reproduce the location of the arcs. The moonlets’ formation is analysed by the disruption of an ancient body at a Lagrangian point of a moon. The disruption fragments spread out in horseshoe orbits and collide to form moonlets, which reach an equilibrium configuration due to a non-conservative effect. In such a scenario, the arcs likely formed through a mixture of different processes, with impacts between disruption outcomes and meteoroid impacts with the moonlets being possibilities.

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Section: Moon Disruption Stagementioning

confidence: 99%

Section: Post-formation Stagementioning

confidence: 99%

Numerical analysis of processes for the formation of moonlets confining the arcs of Neptune

Madeira

Winter

2022

Monthly Notices of the Royal Astronomical Society

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Long-term dynamical evolution of Pallene (Saturn XXXIII) and its diffuse, dusty ring

Muñoz-Gutiérrez

Contreras

Madeira

et al. 2021

Monthly Notices of the Royal Astronomical Society

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The distinctive set of Saturnian small satellites, Aegaeon, Methone, Anthe, and Pallene, constitutes an excellent laboratory to understand the evolution of systems immersed in co-orbital dusty rings/arcs, subjected to perturbations from larger satellites and non-gravitational forces. In this work, we carried out a comprehensive numerical exploration of the long-term evolution of Pallene and its ring. Through frequency map analysis, we characterised the current dynamical state around Pallene. A simple tidal evolution model serves to set a time frame for the current orbital configuration of the system. With detailed short and long-term N-body simulations we determine whether Pallene is currently in resonance with one or more of six of Saturn’s major moons. We analysed a myriad of resonant arguments extracted from the direct and indirect parts of the disturbing function, finding that Pallene is not in mean motion resonance from the present up to 5 Myr into the future; none the less, some resonant arguments exhibit intervals of libration and circulation at different timescales and moon pairings. We studied the dynamical evolution of micrometric particles forming the ring, considering gravitational and non-gravitational forces. Non-gravitational forces are responsible for particles vertical excursions and outward migration. By estimating the satellite’s mass production rate, we find that Pallene could be responsible for keeping its ring in steady-state only if it is mainly composed of large micrometre-sized particles. If mainly composed of particles with a few micrometres for which Pallene is the only source, the ring will spread out, both radially and vertically, until it finally disappears.

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Long-term Dynamical Stability in the Outer Solar System. I. The Regular and Chaotic Evolution of the 34 Largest Trans-Neptunian Objects

Muñoz-Gutiérrez

Peimbert

Lehner

et al. 2021

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We carried out an extensive analysis of the stability of the outer solar system, making use of the frequency analysis technique over short-term integrations of nearly 100,000 test particles, as well as a statistical analysis of 200 1 Gyr long numerical simulations, which consider the mutual perturbations of the giant planets and the 34 largest trans-Neptunian objects (we have called all 34 objects “dwarf planets,” DPs, even if probably only the largest of them are true DPs). From the frequency analysis, we produced statistical diffusion maps for a wide region of the a–e phase-space plane; we also present the average diffusion time for orbits as a function of perihelion. We later turned our attention to the 34 DPs, making an individualized analysis for each of them and producing a first approximation of their future stability. From the 200 distinct realizations of the orbital evolution of the 34 DPs, we classified the sample into three categories, including 17 stable, 11 unstable, and 6 resonant objects; we also found that, statistically, two objects from the sample will leave the trans-Neptunian region within the next gigayear, most likely being ejected from the solar system, but with a nonnegligible probability of going inside the orbit of Neptune, either to collide with a giant planet or even falling to the inner solar system, where our simulations are no longer able to resolve their continuous evolution.

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Analysing the region of the rings and small satellites of Neptune

Cited by 5 publications

References 26 publications

Numerical analysis of processes for the formation of moonlets confining the arcs of Neptune

Numerical analysis of processes for the formation of moonlets confining the arcs of Neptune

Long-term dynamical evolution of Pallene (Saturn XXXIII) and its diffuse, dusty ring

Long-term Dynamical Stability in the Outer Solar System. I. The Regular and Chaotic Evolution of the 34 Largest Trans-Neptunian Objects

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