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

Mauk, B. H.; Mitchell, D. G.; McEntire, R. W.; Paranicas, C.; Roelof, E. C.; Williams, D. J.; Krimigis, S. M.; Lagg, A.

doi:10.1029/2003ja010270

Cited by 245 publications

(356 citation statements)

References 93 publications

(197 reference statements)

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“…Chotoo et al 2000;Mann et al 2002;Zouganelis et al 2004;Maksimovic et al 2005;Marsch 2006; Yoon et al 2006;Pierrard and Lazar 2010), and planetary magnetospheres (e.g. Christon 1987;Collier and Hamilton 1995;Mauk et al 2004;Schippers et al 2008;Dialynas et al 2009;Ogasawara et al 2012), (2) the outer heliosphere and the inner heliosheath (e.g. Decker and Krimigis 2003;Decker et al 2005;Heerikhuisen et al 2008Livadiotis et al 2011Livadiotis et al , 2013Livadiotis and McComas 2012a), and (3) other various plasma-related analyses (e.g.…”

mentioning

confidence: 99%

Understanding Kappa Distributions: A Toolbox for Space Science and Astrophysics

2013

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In this paper we examine the physical foundations and theoretical development of the kappa distribution, which arises naturally from non-extensive Statistical Mechanics. The kappa distribution provides a straightforward replacement for the Maxwell distribution when dealing with systems in stationary states out of thermal equilibrium, commonly found in space and astrophysical plasmas. Prior studies have used a variety of inconsistent, and sometimes incorrect, formulations, which have led to significant confusion about these distributions. Therefore, in this study, we start from the N -particle phase space distribution and develop seven formulations for kappa distributions that range from the most general to several specialized versions that can be directly used with common types of space data. Collectively, these formulations and their guidelines provide a "toolbox" of useful and statistically well-grounded equations for future space physics analyses that seek to apply kappa distributions in data analysis, simulations, modeling, theory, and other work.

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mentioning

confidence: 99%

Understanding Kappa Distributions: A Toolbox for Space Science and Astrophysics

2013

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“…Chotoo et al 2000;Mann et al 2002;Maksimovic et al 2005;Yoon et al 2006;Pierrard and Lazar 2010), planetary magnetospheres (e.g. Christon 1987;Collier and Hamilton 1995;Grabbe 2000;Mauk et al 2004;Schippers et al 2008;Dialynas et al 2009;Ogasawara et al 2013), outer heliosphere and inner heliosheath (e.g. Decker and Krimigis 2003;Decker et al 2005;Heerikhuisen et al 2008;Zank et al 2010;Livadiotis et al 2011Livadiotis et al , 2013, and other general plasma analyses (e.g.…”

Section: Introductionmentioning

confidence: 99%

Electrostatic shielding in plasmas and the physical meaning of the Debye length

Livadiotis

McComas

2014

J. Plasma Phys.

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This paper examines the electrostatic shielding in plasmas, and resolves inconsistencies about what the Debye length really is. Two different interpretations of the Debye length are currently used: (1) The potential energy approximately equals the thermal energy, and (2) the ratio of the shielded to the unshielded potential drops to 1/e. We examine these two interpretations of the Debye length for equilibrium plasmas described by the Boltzmann distribution, and non-equilibrium plasmas (e.g. space plasmas) described by kappa distributions. We study three dimensionalities of the electrostatic potential: 1-D potential of linear symmetry for planar charge density, 2-D potential of cylindrical symmetry for linear charge density, and 3-D potential of spherical symmetry for a point charge. We resolve critical inconsistencies of the two interpretations, including: independence of the Debye length on the dimensionality; requirement for small charge perturbations that is equivalent to weakly coupled plasmas; correlations between ions and electrons; existence of temperature for nonequilibrium plasmas; and isotropic Debye shielding. We introduce a third Debye length interpretation that naturally emerges from the second statistical moment of the particle position distribution; this is analogous to the kinetic definition of temperature, which is the second statistical moment of the velocity distribution. Finally, we compare the three interpretations, identifying what information is required for theoretical/experimental plasma-physics research: Interpretation 1 applies only to kappa distributions; Interpretation 2 is not restricted to any specific form of the ion/electron distributions, but these forms have to be known; Interpretation 3 needs only the second statistical moment of the positional distribution.

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“…In a dipole model of the magnetic field, L (expressed in planetary radii) is the distance at which magnetic field lines associated with that L shell cross the magnetic equator. This plot uses the energy spectra determined by Mauk et al (2004) , who based their fits on time-offlight and other measurements from the Galileo Energetic Particles Detector (EPD) instrument at a limited number of Jovian distances. The data show the peak intensity is located close to the orbit of Europa, falling both inward toward Jupiter and outward toward Callisto.…”

Section: Charged Particle Bombardment Of the Three Outer Galilean Satmentioning

confidence: 99%

“…Hansen and McCord (2004) further found through the analysis of the 1.65 μm water ice feature, that ice grains are crystalline in their interiors such that amorphous ice, when present, is limited to the very top surface. At a depth of 1 mm and deeper, all water ice on these three satellites is crys- These points are derived from fit functions to the Galileo EPD data created by Mauk et al (2004) . Units are protons per cm 2 -s-sr-keV.…”

Section: Introductionmentioning

confidence: 99%

Magnetospheric considerations for solar system ice state

Paranicas¹,

Hibbitts²,

Kollmann³

et al. 2018

Icarus

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a b s t r a c tThe current lattice configuration of the water ice on the surfaces of the inner satellites of Jupiter and Saturn is likely shaped by many factors. But laboratory experiments have found that energetic proton irradiation can cause a transition in the structure of pure water ice from crystalline to amorphous. It is not known to what extent this process is competitive with other processes in solar system contexts. For example, surface regions that are rich in water ice may be too warm for this effect to be important, even if the energetic proton bombardment rate is very high. In this paper, we make predictions, based on particle flux levels and other considerations, about where in the magnetospheres of Jupiter and Saturn the ∼MeV proton irradiation mechanism should be most relevant. Our results support the conclusions of Hansen and McCord (2004), who related relative level of radiation on the three outer Galilean satellites to the amorphous ice content within the top 1 mm of surface. We argue here that if magnetospheric effects are considered more carefully, the correlation is even more compelling. Crystalline ice is by far the dominant ice state detected on the inner Saturnian satellites and, as we show here, the flux of bombarding energetic protons onto these bodies is much smaller than at the inner Jovian satellites. Therefore, the ice on the Saturnian satellites also corroborates the correlation.

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

Cited by 245 publications

References 93 publications

Understanding Kappa Distributions: A Toolbox for Space Science and Astrophysics

Understanding Kappa Distributions: A Toolbox for Space Science and Astrophysics

Electrostatic shielding in plasmas and the physical meaning of the Debye length

Magnetospheric considerations for solar system ice state

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