Dynamics and distribution of Jovian dust ejected from the Galilean satellites

Liu, Xiaodong; Sachse, M.; Spahn, F.; Schmidt, Jürgen

doi:10.1002/2016je004999

Cited by 21 publications

(20 citation statements)

References 64 publications

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“…The time interval ∆t is constant for all trajectories in the whole simulation to ensure that particle positions are stored equidistantly in time. Each storage corresponds to a particle in the simulation (Liu et al 2016).…”

Section: Simulational Schemementioning

confidence: 99%

Dust arcs in the region of Jupiter’s Trojan asteroids

Liu

Schmidt

2018

A&A

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Aims. The surfaces of the Trojan asteroids are steadily bombarded by interplanetary micrometeoroids, which releases ejecta of small dust particles. These particles form the faint dust arcs that are associated with asteroid clouds. Here we analyze the particle dynamics and structure of the arc in the region of the L 4 Trojan asteroids. Methods. We calculate the total cross section of the L 4 Trojan asteroids and the production rate of dust particles. The motion of the particles is perturbed by a variety of forces. We simulate the dynamical evolution of the dust particles, and explore the overall features of the Trojan dust arc. Results. The simulations show that the arc is mainly composed of grains in the size range 4-10 microns. Compared to the L 4 Trojan asteroids, the dust arc is distributed more widely in the azimuthal direction, extending to a range of [30,120] degrees relative to Jupiter. The peak number density does not develop at L 4 . There exist two peaks that are azimuthally displaced from L 4 .

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Section: Simulational Schemementioning

confidence: 99%

Dust arcs in the region of Jupiter’s Trojan asteroids

Liu

Schmidt

2018

A&A

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“…The dynamics of the dust particles in circumjovian space is influenced by various forces, including Jupiter's gravity, the Lorentz force, solar radiation pressure, Poynting-Robertson drag, plasma drag, and the gravity from other celestial bodies. Taking into account all these forces, the equation of motion of a dust grain in the Jovicentric inertial frame reads [49,53,54]…”

Section: Physical Environment For Dust Dynamicsmentioning

confidence: 99%

“…Later, a semi-analytical model was developed to analyze the dynamics and distribution of charged particles in the region of the Galilean moons [84]. High accuracy simulations for a large number of particles of various sizes were performed in [54], including the gravitational J 2 , J 4 and J 6 terms, Lorentz force, solar radiation pressure, Poynting-Robertson drag, plasma drag, and the gravitational perturbations from the Sun and the four Galilean moons; the particle lifetimes, the asymmetry of the dust configuration in the frame rotating with the Sun, the transport of dust between the Galilean moons and to Jupiter, as well as the distribution of orbital elements of the dust grains were investigated.…”

Section: Dust In the Region Of The Galilean Moonsmentioning

confidence: 99%

“…In the region of the Galilean moons there exists an appreciable fraction of particles on retrograde orbits detected by the Galileo DDS [21,83]. The sources of these particles are (1) captured interplanetary and interstellar dust through exchange of energy and angular momentum with the Jovian magnetosphere [21,35,36], (2) particles transported inward from the Jovian outer irregular retrograde moons [80,81], (3) particles from comet Shoemaker-Levy 9 [82], and (4) grains from Galilean moons with large inclinations excited by solar radiation pressure and Lorentz force [54]. Fig.…”

Section: Dust In the Region Of The Galilean Moonsmentioning

confidence: 99%

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Dust in the Jupiter system outside the rings

Liu

Schmidt

2018

Astrodyn

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Jupiter is one of the major targets for planetary exploration, and dust in the Jovian system is of great interest to researchers in the field of planetary science. In this paper, we review the five dust populations outside the ring system: grains in the region of the Galilean moons, potential dust from plumes on Europa, Jovian stream particles, particles in the outer region of the Jovian system ejected from the irregular satellites, and dust in the region of the Trojan asteroids. The physical environment for the dust dynamics is described, including the gravity, the magnetic field and the plasma environment. For each population, the dust sources are described, and the relevant perturbation forces are discussed. Observations and results from modeling are reviewed, and the distributions of the individual dust populations are shown. The understanding of the Jovian dust environment allows to assess the dust hazard to spacecraft, and to characterize the material exchange between the Jovian moons, their surface properties and distribution of non-icy constituents.

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“…Several meteoroid engineering models have been developed for Earth orbit (Smith, 1994;Divine, 1993;Staubach et al, 1997;McNamara et al, 2004;Dikarev et al, 2005) and others for interplanetary space (ibid.). Recently, meteoroid flux models have also been developed for special locations such as for the local Jovian system (Liu et al, 2016), and for special events such as meteor storms (Cooke and Moser, 2010) or a close encounter of Mars with a In literature diverse studies were performed to correct for this bias and different bias correction methods were applied. Since raw brightness-limited (by optical means) or electron-line density limited (by radar) surveys have strong speed biases the final distribution is heavily dependent on assumptions of the mass distribution and luminous or ionization efficiency etc.…”

Section: Introductionmentioning

confidence: 99%

Velocity distribution of larger meteoroids and small asteroids impacting Earth

Drolshagen

Ott

Koschny

et al. 2020

Planetary and Space Science

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Various meteor and fireball networks exist worldwide. Most data sets which include ground-based observational data of meteors are affected by biases. The larger and faster the entering meteoroid, the brighter is the produced meteor. Hence, small and slow objects often stay undetected. This bias of meteor observations towards faster meteoroids is a challenge if quantitative population and flux models are derived. In this work the velocity distribution of objects in space is analysed by using different data sets that are not affected by this velocity bias since they include only large objects, like the near-Earth Oldenburg, 14 November 2019 NEMO-PA-004_1_2_velocity-distributions 2 object (NEO) risk list of ESA's (European Space Agency) SSA (Space Situational Awareness) near-Earth object Coordination Centre (NEOCC), and the fireballs in NASA's (National Aeronautics and Space Administration) CNEOS (Center for near-Earth object Studies) JPL (Jet Propulsion Laboratory) fireball database. Additionally, when only the largest objects recorded with the CILBO (Canary Island Long-Baseline Observatory) camera setup were analysed, a very similar distribution was shown. These velocity distributions are in good agreement with a widely used velocity distribution for smaller sporadic meteoroids in free space which was adopted as reference by the ECSS (European Cooperation for Space Standardisation) Space Environment Standard. cometary coma (Moorhead et al., 2014). The influx of larger objects, starting at a size of a few metres, is relevant for the topic of Planetary Defence, as these may cause damage on our planet. When a meteoroid or small asteroid enters the Earth's Atmosphere it ablates and excites the surrounding air. This leads to a visible meteor or fireball (a meteor brighter than magnitude-4). The brightness of a meteor or fireball depends mainly on the mass and velocity of the impacting object. Especially, it is a strong function of the velocity. This holds true for radar or optical meteors alike. There are various publications and formulas which relate the mass and velocity of the impactor to resulting meteor brightness, see e.g. Verniani (1973), Ceplecha and McCrosky (1976), Halliday et al. (1996), or Weryk and Brown (2013). A common feature of all these formulas is a strong dependence on the impact speed. This strong dependence of the brightness on velocity introduces a clear bias towards meteoroids with higher velocities. This is most obvious for meteor showers which usually have high impact velocities. The enhanced meteor activity during such streams is mainly resulting from the high impact velocity which makes smaller, and more abundant, objects visible as meteors. At lower velocities the meteoroid streams would be hardly noticeable within the sporadic background population. Velocities of meteoroids entering the Earth's Atmosphere can range from about 11 km/s to above 73 km/s. The gravitational attraction of Earth determines the lower limit of this range, particles on interplanetary trajectories hit Earth with spee...

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Dynamics and distribution of Jovian dust ejected from the Galilean satellites

Cited by 21 publications

References 64 publications

Dust arcs in the region of Jupiter’s Trojan asteroids

Dust arcs in the region of Jupiter’s Trojan asteroids

Dust in the Jupiter system outside the rings

Velocity distribution of larger meteoroids and small asteroids impacting Earth

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