Galileo energetic particles detector measurements of hot ions in the neutral sheet region of Jupiter's magnetodisk

Kane, M.; Williams, D. J.; Mauk, B. H.; McEntire, R. W.; Roelof, E. C.

doi:10.1029/1998gl900267

Cited by 33 publications

(30 citation statements)

References 20 publications

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“…The information is obtained by detailed analysis of data obtained by the Energetic Particle Detector (EPD) on the Jupiter‐orbiting Galileo spacecraft for near‐equatorial positions at selected radial positions between ∼6 and ∼46 R J . This report extends and updates previous reports on Galileo EPD composition results [ Williams et al , 1996; Ip et al , 1997, 1998; Mauk et al , 1998; Kane et al , 1999; Cooper et al , 2001; Paranicas et al , 2002, 2003].…”

Section: Introductionsupporting

confidence: 90%

“…The highest‐energy channels are required to quantify spectral moments in the inner magnetosphere, and quality flow anisotropy information is needed to quantify the lowest‐energy portion of the heavy ion spectra where composition‐discriminated channels are not available. Flow information can be derived during the real time mode periods [ Kane et al , 1999; Krupp et al , 2001], but the level of additional analysis required is beyond the scope of the present work.…”

Section: Datamentioning

confidence: 99%

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Energetic ion characteristics and neutral gas interactions in Jupiter's magnetosphere

et al. 2004

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[1] Spectra, integral moments, and composition (H, He, O, S) of energetic ions (50 keV to 50 MeV) are presented for selected Jupiter magnetospheric positions near the equator between radial distances of $6 to $46 Jupiter radii (R J ), as revealed by analysis of the Galileo Energetic Particle Detector data. These characteristics are then used as the basis of interpreting and modeling reported signatures of energetic ion/neutral gas interactions within Jupiter's inner magnetosphere, particularly energetic neutral atom emissions measured during the Cassini spacecraft flyby of Jupiter. Key findings include the following: (1) sulfur ions significantly dominate the energetic (!50 keV) ion density and pressure at all radial distances >7 R J ; (2) protons dominate integral number and energy intensity planetward of 20-25 R J ; (3) a distinct signature of local, equatorial acceleration of energetic protons is revealed between Io (5.9 R J ) and Europa (9.4 R J ); (4) significant spectral and compositional signatures of neutral gas interactions are also revealed between the orbits of Io and Europa; (5) a previously reported significant depletion of ring current ion populations between Io and Europa during the early-phase operation of Galileo ($1995), as compared with observations obtained during the Voyager epoch (1979), has persisted and probably deepened during later Galileo phases (1999); and (6) detailed energetic neutral atom emission modeling, based on the in situ results reported here, further constrains recent estimates of the contents of the neutral gas torus of Europa.

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Section: Introductionsupporting

confidence: 90%

Section: Datamentioning

confidence: 99%

Energetic ion characteristics and neutral gas interactions in Jupiter's magnetosphere

et al. 2004

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“…Thermal protons and heavy ions in Mercury's magnetotail (e.g., Na + ) have energies around ∼2.5 keV and ∼1 keV [ Jackman et al , ; Gershman et al , ]. The plasma content in Jupiter's magnetosphere represents a mixture of protons with energy ∼10 keV and sulfur ions S + with energy ∼45 keV [ Frank et al , ; Kane et al , ]. Direct spacecraft measurements have shown the increase of fluxes of high‐energy protons and ions in the vicinity of plasma jets both in the Earth's [ Luo et al , ] and Jupiter's magnetotail [ Kasahara et al , ; Artemyev et al , ].…”

Section: Introductionmentioning

confidence: 99%

Heavy ion acceleration at dipolarization fronts in planetary magnetotails

Greco

Artemyev

Zimbardo

2015

Geophys. Res. Lett.

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Transient reconnection events in planetary magnetotails give rise to fast plasma jets, whose leading edges are called dipolarization fronts. We perform a test particle simulation of the acceleration of several ion species (H+, He+, and O+) in a 2‐D model of dipolarization fronts. We study the dependence of the acceleration on parameters of the model, finding, e.g., that the average ion energy increases with the front velocity and with the initial injection energy. When the ion species are initially cold, O+ ions get the largest amount of average energy. Conversely, when the injection energy of O+ ions is increased, their average energy gain does not exceed that of the lighter species, suggesting that ion energization at local dipolarization fronts strongly depends on the initial particle gyroradius. Further, the energy gained by the most energetic fraction of particles scales approximately as the square root of the mass ratio.

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“…The outward transport of mass means that in steady state there must also be outward transport of angular momentum. Moreover, everywhere one expects some departure from corotation with greater departure at large radial distances [Kane et al, 1999, and references therein]. In Hill's [1979] picture the outward mass transport in the magnetosphere requires that there be a continual supply of angular momentum from the planet.…”

Section: Introductionmentioning

confidence: 99%

A new perspective concerning the influence of the solar wind on the Jovian magnetosphere

Southwood¹,

Kivelson²

2001

J. Geophys. Res.

158

187

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Abstract. The solar wind exerts a strong influence on the Jovian magnetosphere in changing its volume, in energizing plasma, and in stimulating the aurora and a host of other associated effects. However, whereas at Earth the dominant solar terrestrial coupling process is magnetic reconnection, the dominant energy reservoir in Jupiter's magnetospheric plasma, continually present, is the kinetic energy of its rotating plasma disk. This "flywheel"' produces effects with no terrestrial analogy, some of which we describe here. The most surprising prediction from the analysis of this paper is that remotely sensed symptoms of Jovian magnetospheric activity are likely to occur in conjunction with solar wind pressure decreases. Compressions of the magnetosphere produced by forward shocks and other solar wind pressure increases will heat the magnetospheric plasma but substantially reduce the ionosphere-magnetosphere current systems. The intensity of dayside aurora and of radio wave emissions associated with increased ionospheric-magnetospheric current systems will tend to anticorrelate with magnetospheric compressions and correlate with expansions. The link to the aurora is based on an argument that the auroral zone maps to the plasma disk of the middle magnetosphere and is thus linked to plasma sheet dynamics. The effect of expansion on the plasma sheet is to increase the parallel pressure, setting up conditions that can produce detached plasma "blobs" and enhance mass loss. The analysis is particularly apposite in light of the opportunities for observing solar wind-Jovian interactions using data from both the Galileo and the Cassini spacecraft during the Cassini flyby of Jupiter in late 2000, ideally supplemented by auroral imaging with ground-based and Hubble telescopes.

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Galileo energetic particles detector measurements of hot ions in the neutral sheet region of Jupiter's magnetodisk

Cited by 33 publications

References 20 publications

Energetic ion characteristics and neutral gas interactions in Jupiter's magnetosphere

Energetic ion characteristics and neutral gas interactions in Jupiter's magnetosphere

Heavy ion acceleration at dipolarization fronts in planetary magnetotails

A new perspective concerning the influence of the solar wind on the Jovian magnetosphere

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