Orbital evolution of the<i>μ</i>and<i>ν</i>dust ring particles of Uranus

Sfair, R.; Winter, S. M. Giuliatti

doi:10.1051/0004-6361/200911886

Cited by 9 publications

(9 citation statements)

References 79 publications

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“…The effects of the other two remaining perturbations, the planetary oblateness and the solar radiation pressure, were addressed in a previous paper (Sfair & Giuliatti Winter 2009). Using numerical simulations, we analysed the combined effect of both forces on the orbital evolution of an ensemble of micrometic particles evenly spaced across the radial extension of the μ ring, taking into account the gravitational perturbation of Puck and Mab.…”

Section: Disturbing Forcesmentioning

confidence: 99%

“…To mimic the scenario in which Mab is the source the of ring dust particles, we studied the dynamics of grains initially ejected from the satellite, which is different from the initial conditions of Sfair & Giuliatti Winter (2009).…”

Section: Initial Conditions and Numerical Modelmentioning

confidence: 99%

“…Our model also includes the components of the solar radiation force (SRF) as described in Sfair & Giuliatti Winter (2009), assuming particles of ideal material. Effects of planetary shadow and of the light reflected from the planet were not taken into account, since their contribution to the evolution of the particles is secondary when compared to the effects of direct illumination (Hamilton 1993).…”

Section: Initial Conditions and Numerical Modelmentioning

confidence: 99%

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The role of Mab as a source for theμring of Uranus

Sfair

Winter

2012

A&A

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Context. We previously analysed how the solar radiation force combined with the planetary oblateness changes the orbital evolution of a sample of dust particles located at the secondary ring system of Uranus. Both effects combined with the gravitational perturbations of the close satellites lead to the depletion of these dust particles through collisions on the surfaces of these satellites on a timescale of hundreds of years. Aims. In this work we investigate if the impacts of interplanetary dust particles (IDPs) onto Mab's surface can produce sufficient particles to replenish the μ ring population. Methods. We first analysed through numerical simulations the evolution of a sample of particles ejected from the surface of Mab and computed the lifetime of the grains when the effects of the solar radiation pressure and the planetary oblateness are taken into account. Then we estimated the mass production rate due to the impacts of IDPs following a previously established algorithm, and used this value to determine the time necessary to accumulate an amount of particles comparable with the mass of the μ ring. Results. Based on an estimate of the flux of interplanetary particles and on the surface properties of Mab it is expected that the satellite supplies material to the ring at a rate of ∼3 g/s. Meanwhile, our numerical model showed that the ejected particles are removed from the system through collisions with the satellite, and the mean lifetime of the grains may vary from 320 to 1500 years, depending on the radius of the particle. Conclusions. The time necessary to accumulate the mass of the μ ring via ejection from Mab is much shorter than the mean lifetime of the particles, and a stationary regime is not reached. If the ring is kept in a steady state, other effects such as the electromagnetic force and/or the existence of additional bodies may play a significant role in the dust balance, but the current lack of information about the environment renders modelling these effects unfeasible.

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Section: Disturbing Forcesmentioning

confidence: 99%

Section: Initial Conditions and Numerical Modelmentioning

confidence: 99%

Section: Initial Conditions and Numerical Modelmentioning

confidence: 99%

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The role of Mab as a source for theμring of Uranus

Sfair

Winter

2012

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“…In brief, the pericentre precession caused by the highly oblate central body protects the very small grains against the strong solar radiation pressure, e.g. Sfair & Giuliatti (2009), and keeps them bounded. And vice-versa, RP excites the eccentricity of individual ring inhabitants helping to align their apses.…”

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Dynamics of Haumea’s dust ring

Regály

2018

Monthly Notices of the Royal Astronomical Society

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The particle dynamics of the recently observed ring around dwarf planet Haumea is numerically investigated. The point mass gravitational force, a second degree and order gravity field, and the solar radiation pressure as the main perturbations are considered. The quasi-stationary state of the ring varies for different micron-sized grains and depends also on the spin-orbit resonances between the rotation rate of the main body and the orbital period of the dust particles. The simulations confirm the variable radial width of the ring observed during the transit ingress and egress. Results show that the micron sized grains, initially on circular orbits, become eccentric and form an apse-aligned ring at the observed radial distance near to the 3:1 spinorbit resonance. It is also demonstrated that this coincidence is only apparent and independent of 3:1 resonance.

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“…Também não foram verificadas colisões entre as partículas e o planeta. Sfair et al (2009) analisaram o movimento de partículas com raios iguais a 1μm, 3μm, 5μm e 10μm localizadas na região do anel F de Saturno sob os efeitos da pressão de radiação. Como resultado foi obtido que partículas com 1μm de raio alcançaram uma excentricidade máxima de ∼0,60 e colidiram com Saturno em menos de 10 anos.…”

Section: Análise Dos Resultadosunclassified

Análise da estabilidade da região externa do sistema Plutão-Caronte após a descoberta dos novos satélites NIX e HIDRA

Santos¹

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In this work we performed a numerical analysis of the the outer region of the Pluto-Charon system by the insertion of a sample of test particles initially in P-type prograde and retrograde orbits, in the system formed by Pluto, Charon, Nix and Hydra. These numerical integrations generated diagrams of semi-major axis versus eccentricity which define regions of particles in stable orbits and regions of collision and escape. In the vicinity of the satellites Nix and Hydra were identified chaotic regions, where particles located in this region have their eccentricities and semi-major axis increased provoking an ejection or collision with a massive body of the system. A set of particles remained in regions near the orbits of Nix and Hydra, possibly coorbitais with them. For both cases, prograde and retrograde, the "stable" region is larger in the outer region of the system, after Hydra's orbit, depending on the value of eccentricity. Numerical simulations were also performed by inserting some massive hypothetical satellites beyond the Charon's orbit and the effects on the orbits of Nix and Hydra were analyzed. A preliminary numerical study of the effects of the solar radiation force on a sample of particles with radii of 1μm, 3μm, 5μm e 10μm was performed. This study showed that particles under the effects of the Poynting-Robertson drag decay on a time scale between 1.45 × 10 6 years (particles of 1μm in radius) and 1.45×10 7 years (particles of 10μm in radius), while the radiation pressure caused variations of the eccentricities of the particles causing in some cases collisions with the planet.

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Orbital evolution of theμandνdust ring particles of Uranus

Cited by 9 publications

References 79 publications

The role of Mab as a source for theμring of Uranus

The role of Mab as a source for theμring of Uranus

Dynamics of Haumea’s dust ring

Análise da estabilidade da região externa do sistema Plutão-Caronte após a descoberta dos novos satélites NIX e HIDRA

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