Wave-particle-interaction in kinetic plasmas

Schreiner, Cedric; Spanier, F.

doi:10.1016/j.cpc.2014.03.028

Cited by 13 publications

(19 citation statements)

References 11 publications

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“…On the other hand , there are many approaches to study the bow shock location, dynamics and physical properties, such as Hybrid models 24,46,55 ,MHD models 33,56,60,64 , and PIC models ( 4,57,58,62 ) and the references therein.…”

Section: Introductionmentioning

confidence: 99%

Large Scale Earth’s Bow Shock with Northern IMF as Simulated by PIC Code in Parallel with MHD Model

Baraka¹

2016

J Astrophys Astron

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International audienceIn this paper, we propose a 3D kinetic model (particle-in-cell, PIC) for the description of the large scale Earth’s bow shock. The proposed version is stable and does not require huge or extensive computer resources. Because PIC simulations work with scaled plasma and field parameters, we also propose to validate our code by comparing its results with the available MHD simulations under same scaled solar wind (SW) and (IMF) conditions. We report new results from the two models. In both codes the Earth’s bow shock position is found to be ≈14.8 R E along the Sun–Earth line, and ≈29 R E on the dusk side. Those findings are consistent with past in situ observations. Both simulations reproduce the theoretical jump conditions at the shock. However, the PIC code density and temperature distributions are inflated and slightly shifted sunward when compared to the MHD results. Kinetic electron motions and reflected ions upstream may cause this sunward shift. Species distributions in the foreshock region are depicted within the transition of the shock (measured ≈2 c/ω pi for Θ Bn = 90° and M MS = 4.7) and in the downstream. The size of the foot jump in the magnetic field at the shock is measured to be (1.7c/ω pi ). In the foreshocked region, the thermal velocity is found equal to 213 km s−1 at 15R E and is equal to 63 km s −1 at 12 R E (magnetosheath region). Despite the large cell size of the current version of the PIC code, it is powerful to retain macrostructure of planets magnetospheres in very short time, thus it can be used for pedagogical test purposes. It is also likely complementary with MHD to deepen our understanding of the large scale magnetosphere

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Section: Introductionmentioning

confidence: 99%

Large Scale Earth’s Bow Shock with Northern IMF as Simulated by PIC Code in Parallel with MHD Model

Baraka¹

2016

J Astrophys Astron

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“…However, damped waves can still be studied if a decent amount of energy is artificially deposited in the electromagnetic fields of this wave. For doing so, we employ the initialization mechanism outlined in [3] which excites one or more specific waves at the start of the simulation. Using this method, wave excitation is achieved in three steps: First, the frequency of a wave with wave number k is computed using the cold plasma dispersion relation (e.g.…”

Section: Basic Setupmentioning

confidence: 99%

Recovering the Damping Rates of Cyclotron Damped Plasma Waves from Simulation Data

Schreiner

Kilian

Spanier

2017

Commun. Comput. Phys.

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Plasma waves with frequencies close to the particular gyrofrequencies of the charged particles in the plasma lose energy due to cyclotron damping. We briefly discuss the gyro-resonance of low frequency plasma waves and ions particularly with regard to particle-in-cell (PiC) simulations. A setup is outlined which uses artificially excited waves in the damped regime of the wave mode's dispersion relation to track the damping of the wave's electromagnetic fields. Extracting the damping rate directly from the field data in real or Fourier space is an intricate and non-trivial task. We therefore present a simple method of obtaining the damping rate Γ from the simulation data. This method is described in detail, focusing on a step-by-step explanation of the course of actions. In a first application to a test simulation we find that the damping rates obtained from this simulation generally are in good agreement with theoretical predictions. We then compare the results of one-, two-and three-dimensional simulation setups and simulations with different physical parameter sets.

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“…Nonetheless most numerical simulations cover only the interaction of protons with magnetic fluctuations. With our work we attempt to transfer the approach to analyzing proton scattering with fully kinetic particle-in-cell (PiC) simulations [3] to a setup where the scattering of electrons and dispersive waves can be studied.…”

Section: Introductionmentioning

confidence: 99%

Effects of dispersive wave modes on charged particles transport

Schreiner¹,

Spanier²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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The transport of charged particles in the heliosphere and the interstellar medium is governed by the interaction of particles and magnetic irregularities. For the transport of protons a rather simple model using a linear Alfvén wave spectrum which follows the Kolmogorov distribution usually yields good results. Even magnetostatic spectra may be used. For the case of electron transport, particles will resonate with the high-k end of the spectrum. Here the magnetic fluctuations do not follow the linear dispersion relation, but the kinetic regime kicks in. We will discuss the interaction of fluctuations of dispersive waves in the kinetic regime using a particle-in-cell code [1]. Especially the scattering of particles following the idea of Lange et al. [2] and its application to PiC codes [3] will be discussed. The effect of the dispersive regime on the electron transport will be discussed in detail.

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Wave-particle-interaction in kinetic plasmas

Cited by 13 publications

References 11 publications

Large Scale Earth’s Bow Shock with Northern IMF as Simulated by PIC Code in Parallel with MHD Model

Large Scale Earth’s Bow Shock with Northern IMF as Simulated by PIC Code in Parallel with MHD Model

Recovering the Damping Rates of Cyclotron Damped Plasma Waves from Simulation Data

Effects of dispersive wave modes on charged particles transport

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