The size distribution of Jupiter's main ring from Galileo imaging and spectroscopy

Brooks, S. M.; Esposito, L. W.; Showalter, M. R.; Throop, H. B.

doi:10.1016/j.icarus.2004.03.003

Cited by 23 publications

(23 citation statements)

References 43 publications

(125 reference statements)

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“…This shows that the size distribution extends to particles one order of magnitude smaller than derived from ring images. On the other hand, the largest sizes agree rather well with particle sizes deduced from imaging of the gossamer ring (Showalter et al, 1985;Showalter et al, 2008;de Pater et al, 2008) and Jupiter's main ring Brooks et al, 2004). The only other information on ring particle sizes comes from three impacts detected at ring plane crossing by the Pioneer 10 and Pioneer 11 spacecraft (Humes, 1976).…”

Section: Grain Massessupporting

confidence: 63%

“…Therefore, the in-situ measurements and the imaging results complement each other with only little overlap in the sensitive size range. Furthermore, a size distribution for the main jovian ring was recently determined from Galileo observations by Brooks et al (2004). They find a power law slope of À2.0 ± 0.3 for particles below $15 lm and a transition to a power law with slope À5.0 ± 1.5 at larger sizes.…”

Section: Amalthea Ring Thebe Ring Uncertaintymentioning

confidence: 98%

“…13 shows that the small grains measured in-situ represent only a minor fraction of the total ring mass contained in the dust: Assuming that the size distribution for optically visible grains in the size range 4-30 lm measured by Showalter et al (2008) is valid for all gossamer rings, the total ring mass is increased by a factor of $30 over the values for small particles that we list in Table 3. Similarly, if we take the bimodal size distribution derived for the main jovian ring by Brooks et al (2004) in the size range 0.1-100 lm, the gossamer ring mass increases by a factor of $25. There is evidence for even more mass at still greater sizes .…”

Section: Total Ring Massmentioning

confidence: 99%

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Galileo in-situ dust measurements in Jupiter’s gossamer rings

Krüger

Hamilton

Moissl

et al. 2009

Icarus

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a b s t r a c tGalileo was the first artificial satellite to orbit Jupiter. During its late orbital mission the spacecraft made two passages through the giant planet's gossamer ring system. The impact-ionization dust detector on board successfully recorded dust impacts during both ring passages and provided the first in-situ measurements from a dusty planetary ring. During the first passage-on 5 November 2002 while Galileo was approaching Jupiter-dust measurements were collected until a spacecraft anomaly at 2.33R J (Jupiter radii) just 16 min after a close flyby of Amalthea put the spacecraft into a safing mode. The second ring passage on 21 September 2003 provided ring dust measurements down to about 2.5R J and the Galileo spacecraft was destroyed shortly thereafter in a planned impact with Jupiter. In all, a few thousand dust impacts were counted with the instrument accumulators during both ring passages, but only a total of 110 complete data sets of dust impacts were transmitted to Earth. Detected particle sizes range from about 0.2 to 5 lm, extending the known size distribution by an order of magnitude towards smaller particles than previously derived from optical imaging [Showalter, M.R., de Pater, I., Verbanac, G., Hamilton, D.P., Burns, J.A., 2008. Icarus 195, 361-377; de Pater, I., Showalter, M.R., Macintosh, B., 2008. Icarus 195, 348-360]. The grain size distribution increases towards smaller particles and shows an excess of these tiny motes in the Amalthea gossamer ring compared to the Thebe ring. The size distribution for the Amalthea ring derived from our in-situ measurements for the small grains agrees very well with the one obtained from images for large grains. Our analysis shows that particles contributing most to the optical cross-section are about 5 lm in radius, in agreement with imaging results. The measurements indicate a large drop in particle flux immediately interior to Thebe's orbit and some detected particles seem to be on highly-tilted orbits with inclinations up to 20°. Finally, the faint Thebe ring extension was detected out to at least 5R J , indicating that grains attain higher eccentricities than previously thought. The drop interior to Thebe, the excess of submicron grains at Amalthea, and the faint ring extension indicate that grain dynamics is strongly influenced by electromagnetic forces. These findings can all be explained by a shadow resonance as detailed by Hamilton and Krüger [Hamilton, D.P., Krüger, H., 2008. Nature 453, 72-75].

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Section: Grain Massessupporting

confidence: 63%

Section: Amalthea Ring Thebe Ring Uncertaintymentioning

confidence: 98%

Section: Total Ring Massmentioning

confidence: 99%

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Galileo in-situ dust measurements in Jupiter’s gossamer rings

Krüger

Hamilton

Moissl

et al. 2009

Icarus

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“…Earlier images from Voyager and Galileo showed longitudinal asymmetries on a scale much larger than the tiny clumps found by New Horizons (6,7,12). The absence such large features in the recent data is puzzling; perhaps seasonal or other time-scale variations play a role.…”

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confidence: 87%

Clump Detections and Limits on Moons in Jupiter's Ring System

Showalter

Cheng

Weaver

et al. 2007

Science

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The dusty jovian ring system must be replenished continuously from embedded source bodies. The New Horizons spacecraft has performed a comprehensive search for kilometer-sized moons within the system, which might have revealed the larger members of this population. No new moons were found, however, indicating a sharp cutoff in the population of jovian bodies smaller than 8-kilometer-radius Adrastea. However, the search revealed two families of clumps in the main ring: one close pair and one cluster of three to five. All orbit within a brighter ringlet just interior to Adrastea. Their properties are very different from those of the few other clumpy rings known; the origin and nonrandom distribution of these features remain unexplained, but resonant confinement by Metis may play a role.

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“…bution is considerably steeper (richer in small particles) than previously believed (McMuldroch et al 2000, Brooks et al 2003. The Planetary Data System Discipline Node for Planetary Rings was established and has become a repository for a large amount of archival information on ring systems, including that noted above ; http://ringmaster.arc.…”

Section: Introduction and Overviewmentioning

confidence: 98%

Saturn’s Rings: Pre-Cassini Status and Mission Goals

Cuzzi¹,

Colwell²,

Esposito³

et al. 2003

The Cassini-Huygens Mission

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Abstract. Theoretical and observational progress in studies of Saturn's ring system since the mid1980s is reviewed, focussing on advances in configuration and dynamics, composition and size distribution, dust and meteoroids, interactions of the rings with the planet and the magnetosphere, and relationships between the rings and various satellites. The Cassini instrument suite of greatest relevance to ring studies is also summarized, emphasizing how the individual instruments might work together to solve outstanding problems. The Cassini tour is described from the standpoint of ring studies, and major ring science goals are summarized.

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The size distribution of Jupiter's main ring from Galileo imaging and spectroscopy

Cited by 23 publications

References 43 publications

Galileo in-situ dust measurements in Jupiter’s gossamer rings

Galileo in-situ dust measurements in Jupiter’s gossamer rings

Clump Detections and Limits on Moons in Jupiter's Ring System

Saturn’s Rings: Pre-Cassini Status and Mission Goals

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