Test charge response for a dusty plasma with both grain size distribution and dynamical charging

Raadu, Michael A.; Shafiq, Muhammad

doi:10.1063/1.2431354

Cited by 21 publications

(5 citation statements)

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“…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. Milovanov and Zelenyi 2000;Saito et al 2000;Leubner 2004;Raadu and Shafiq 2007;Baluku et al 2010;Livadiotis and McComas 2009, 2010a, 2011bLe Roux et al 2010;Eslami et al 2011;Kourakis et al 2012; see also the work of Tribeche and collaborators in dusty plasmas, e.g., Tribeche et al 2009Tribeche and Bacha 2010;Tribeche and Merriche 2011;Roy et al 2012;Bains et al 2013). Because BG Statistical Mechanics cannot adequately describe non-equilibrium plasmas, new advances were required.…”

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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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confidence: 99%

Understanding Kappa Distributions: A Toolbox for Space Science and Astrophysics

2013

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“…The physical meaning of the Debye length 343 2001; Saito et al 2000;Leubner 2004;Raadu and Shafiq 2007;Hellberg et al 2009;Livadiotis and McComas 2009, 2010a-c, 2011a, 2011b, 2012, 2013aTribeche et al 2009;Le Roux et al 2010;Eslami et al 2011;Kourakis et al 2012;Yoon 2012;Yoon et al 2012;Bains et al 2013;Saberian and Esfandyari-Kalejahi 2013).…”

Section: And Zelenyi 2000mentioning

confidence: 99%

“…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. Milovanov and Zelenyi 2000, The physical meaning of the Debye length 343 2001; Saito et al 2000;Leubner 2004;Raadu and Shafiq 2007;Hellberg et al 2009;Livadiotis and McComas 2009, 2010a-c, 2011a, 2011b, 2012, 2013aTribeche et al 2009;Le Roux et al 2010;Eslami et al 2011;Kourakis et al 2012;Yoon 2012;Yoon et al 2012;Bains et al 2013;Saberian and Esfandyari-Kalejahi 2013).…”

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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“…Kappa distributions are characterized by their high energy tail which is not always clearly observed because of the low plasma intensities in the high energy range. Nevertheless, many analyses used successfully kappa distributions to describe observations in several plasma environments, where the Maxwell distribution clearly fails to describe the high energy tails of the observed distributions: solar wind (e.g., Maksimovic et al 1997;Pierrard et al 1999;Chotoo et al 2000;Mann et al 2002;Marsch 2006;Zouganelis et al 2008;Štverák et al 2009;Livadiotis and McComas 2013b;Yoon 2014;Heerikhuisen et al 2015;Pierrard and Pieters 2015), planetary magnetospheres (e.g., Christon 1987;Collier and Hamilton 1995;Jurac et al 2002;Pisarenko et al 2002;Kletzing et al 2003;Mauk et al 2004;Schippers et al 2008;Dialynas et al 2009;Ogasawara et al 2012;Carbary et al 2014;Qureshi et al 2015;Stepanova and Antonova 2015), the outer heliosphere and the inner heliosheath (e.g., Decker and Krimigis 2003;Decker et al 2005;Heerikhuisen et al 2008;Zank et al 2010;Livadiotis et al 2011;2012;Livadiotis and McComas 2011a;2012), and other various plasma-related analyses (e.g., Milovanov and Zelenyi 2000;Saito et al 2000;Yoon et al 2006;Raadu and Shafiq 2007;Tribeche et al 2009;Hellberg et al 2009;Livadiotis and McComas 2009;…”

Section: Introductionmentioning

confidence: 99%

Misestimation of temperature when applying Maxwellian distributions to space plasmas described by kappa distributions

Nicolaou

Livadiotis

2016

Astrophys Space Sci

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This paper presents the misestimation of temperature when observations from a kappa distributed plasma are analyzed as a Maxwellian. One common method to calculate the space plasma parameters is by fitting the observed distributions using known analytical forms. More often, the distribution function is included in a forward model of the instrument's response, which is used to reproduce the observed energy spectrograms for a given set of plasma parameters. In both cases, the modeled plasma distribution fits the measurements to estimate the plasma parameters. The distribution function is often considered to be Maxwellian even though in many cases the plasma is better described by a kappa distribution. In this work we show that if the plasma is described by a kappa distribution, the derived temperature assuming Maxwell distribution can be significantly off. More specifically, we derive the plasma temperature by fitting a Maxwell distribution to pseudo-data produced by a kappa distribution, and then examine the difference of the derived temperature as a function of the kappa index.We further consider the concept of using a forward model of a typical plasma instrument to fit its observations. We find that the relative error of the derived temperature is highly depended on the kappa index and occasionally on the instrument's field of view and response.

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Test charge response for a dusty plasma with both grain size distribution and dynamical charging

Cited by 21 publications

References 21 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

Misestimation of temperature when applying Maxwellian distributions to space plasmas described by kappa distributions

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