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Journal articles on the topic 'HPC plasma turbulence simulations'

Author: Grafiati

Published: 8 June 2024

Last updated: 31 July 2025

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1

Bouzat, Nicolas, Camilla Bressan, Virginie Grandgirard, Guillaume Latu, and Michel Mehrenberger. "Targeting Realistic Geometry in Tokamak Code Gysela." ESAIM: Proceedings and Surveys 63 (2018): 179–207. http://dx.doi.org/10.1051/proc/201863179.

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In magnetically confined plasmas used in Tokamak, turbulence is respon-sible for specific transport that limits the performance of this kind of reactors. Gyroki-netic simulations are able to capture ion and electron turbulence that give rise to heat losses, but require also state-of-the-art HPC techniques to handle computation costs. Such simulations are a major tool to establish good operating regime in Tokamak such as ITER, which is currently being built. Some of the key issues to address more re- alistic gyrokinetic simulations are: efficient and robust numerical schemes, accurate geometric

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2

Veltri, P., G. Nigro, F. Malara, V. Carbone, and A. Mangeney. "Intermittency in MHD turbulence and coronal nanoflares modelling." Nonlinear Processes in Geophysics 12, no. 2 (2005): 245–55. http://dx.doi.org/10.5194/npg-12-245-2005.

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Abstract. High resolution numerical simulations, solar wind data analysis, and measurements at the edges of laboratory plasma devices have allowed for a huge progress in our understanding of MHD turbulence. The high resolution of solar wind measurements has allowed to characterize the intermittency observed at small scales. We are now able to set up a consistent and convincing view of the main properties of MHD turbulence, which in turn constitutes an extremely efficient tool in understanding the behaviour of turbulent plasmas, like those in solar corona, where in situ observations are not ava

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3

Sharma, A. Y., M. D. J. Cole, T. Görler, et al. "Global gyrokinetic study of shaping effects on electromagnetic modes at NSTX aspect ratio with ad hoc parallel magnetic perturbation effects." Physics of Plasmas 29, no. 11 (2022): 112503. http://dx.doi.org/10.1063/5.0106925.

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Plasma shaping may have a stronger effect on global turbulence in tight-aspect-ratio tokamaks than in conventional-aspect-ratio tokamaks due to the higher toroidicity and more acute poloidal asymmetry in the magnetic field. In addition, previous local gyrokinetic studies have shown that it is necessary to include parallel magnetic field perturbations in order to accurately compute growth rates of electromagnetic modes in tight-aspect-ratio tokamaks. In this work, the effects of elongation and triangularity on global, ion-scale, linear electromagnetic modes are studied at National Spherical Tor

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4

Wang, Bei, Stephane Ethier, William Tang, et al. "Modern gyrokinetic particle-in-cell simulation of fusion plasmas on top supercomputers." International Journal of High Performance Computing Applications 33, no. 1 (2017): 169–88. http://dx.doi.org/10.1177/1094342017712059.

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The gyrokinetic toroidal code at Princeton (GTC-P) is a highly scalable and portable particle-in-cell (PIC) code. It solves the 5-D Vlasov–Poisson equation featuring efficient utilization of modern parallel computer architectures at the petascale and beyond. Motivated by the goal of developing a modern code capable of dealing with the physics challenge of increasing problem size with sufficient resolution, new thread-level optimizations have been introduced as well as a key additional domain decomposition. GTC-P’s multiple levels of parallelism, including internode 2-D domain decomposition and

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5

Cranmer, Steven R., and Momchil E. Molnar. "Magnetohydrodynamic Mode Conversion in the Solar Corona: Insights from Fresnel-like Models of Waves at Sharp Interfaces." Astrophysical Journal 955, no. 1 (2023): 68. http://dx.doi.org/10.3847/1538-4357/acee6c.

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Abstract The solar atmosphere is known to contain many different types of wave-like oscillation. Waves and other fluctuations (e.g., turbulent eddies) are believed to be responsible for at least some of the energy transport and dissipation that heats the corona and accelerates the solar wind. Thus, it is important to understand the behavior of magnetohydrodynamic (MHD) waves as they propagate and evolve in different regions of the Sun’s atmosphere. In this paper, we investigate how MHD waves can affect the overall plasma state when they reflect and refract at sharp, planar interfaces in densit

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Mininni, Pablo. "Harnessing HPC to Understand Turbulence: Capturing the Fine-grain Structure of Geophysical Flows." Resúmenes de Mecánica Computacional 1, no. 2 (2024): 25. https://doi.org/10.70567/rmc.v1i2.144.

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In the realm of atmospheric dynamics, the emergence of large-scale structures from small-scale turbulent convective motions stands as one of the most striking phenomena in nature. This process, which impacts climate modeling, small-scale collisions of particles and droplets in clouds, and has implications for industrial flows, is difficult to capture in traditional turbulence models. This presentation will delve into insights from single- and multi-phase numerical simulations of unprecedented sizes, resolving atmospheric flows with spatial resolutions down to 30 meters. Turbulence in these sim

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Dudson, B. D., and J. Leddy. "Hermes: global plasma edge fluid turbulence simulations." Plasma Physics and Controlled Fusion 59, no. 5 (2017): 054010. http://dx.doi.org/10.1088/1361-6587/aa63d2.

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8

Grandgirard, V., Y. Sarazin, P. Angelino, et al. "Global full-fgyrokinetic simulations of plasma turbulence." Plasma Physics and Controlled Fusion 49, no. 12B (2007): B173—B182. http://dx.doi.org/10.1088/0741-3335/49/12b/s16.

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9

Pueschel, M. J., M. Kammerer, and F. Jenko. "Gyrokinetic turbulence simulations at high plasma beta." Physics of Plasmas 15, no. 10 (2008): 102310. http://dx.doi.org/10.1063/1.3005380.

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10

Edyvean, Jago, Tulasi N. Parashar, Tom Simpson, et al. "Scale Separation Effects on Simulations of Plasma Turbulence." Astrophysical Journal 972, no. 2 (2024): 173. http://dx.doi.org/10.3847/1538-4357/ad5cf5.

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Abstract Understanding plasma turbulence requires a synthesis of experiments, observations, theory, and simulations. In the case of kinetic plasmas such as the solar wind, the lack of collisions renders the fluid closures such as viscosity meaningless and one needs to resort to higher-order fluid models or kinetic models. Typically, the computational expense in such models is managed by simulating artificial values of certain parameters such as the ratio of the Alfvén speed to the speed of light (v A/c) or the relative mass ratio of ions and electrons (m i /m e ). Although, typically care is t

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11

Thyagaraja, A. "Direct Numerical Simulations of Two-Fluid Plasma Turbulence." Le Journal de Physique IV 05, no. C6 (1995): C6–105—C6–108. http://dx.doi.org/10.1051/jp4:1995621.

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12

Galassi, Davide, Guido Ciraolo, Patrick Tamain, et al. "Tokamak Edge Plasma Turbulence Interaction with Magnetic X-Point in 3D Global Simulations." Fluids 4, no. 1 (2019): 50. http://dx.doi.org/10.3390/fluids4010050.

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Turbulence in the edge plasma of a tokamak is a key actor in the determination of the confinement properties. The divertor configuration seems to be beneficial for confinement, suggesting an effect on turbulence of the particular magnetic geometry introduced by the X-point. Simulations with the 3D fluid turbulence code TOKAM3X are performed here to evaluate the impact of a diverted configuration on turbulence in the edge plasma, in an isothermal framework. The presence of the X-point is found, locally, to affect both the shape of turbulent structures and the amplitude of fluctuations, in quali

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13

Janhunen, Salomon, Gabriele Merlo, Alexey Gurchenko, Evgeniy Gusakov, Frank Jenko, and Timo Kiviniemi. "Simulation of transport in the FT-2 tokamak up to the electron scale with GENE." Plasma Physics and Controlled Fusion 64, no. 1 (2021): 015005. http://dx.doi.org/10.1088/1361-6587/ac318c.

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Abstract Prior experimental work on the FT-2 tokamak has observed electron density fluctuations at electron Larmor radius scales using the enhanced scattering (ES) diagnostic (Gusakov et al 2006 Plasma Phys. Control. Fusion 48 A371–6, Gurchenko and Gusakov 2010 Plasma Phys. Control. Fusion 52 124035). Gyrokinetic GENE simulations of conditions at the upper hybrid resonance layer probed by the ES diagnostic show the presence of the anticipated turbulence from the electron temperature gradient (ETG) driven instability in linear and nonlinear simulations. Ion-scale turbulence is responsible for m

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14

Xu, X. Q., W. M. Nevins, R. H. Cohen, J. R. Myra, and P. B. Snyder. "Dynamical simulations of boundary plasma turbulence in divertor geometry." New Journal of Physics 4 (July 24, 2002): 53. http://dx.doi.org/10.1088/1367-2630/4/1/353.

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15

Henriksson, S. V., S. J. Janhunen, T. P. Kiviniemi, and J. A. Heikkinen. "Global spectral investigation of plasma turbulence in gyrokinetic simulations." Physics of Plasmas 13, no. 7 (2006): 072303. http://dx.doi.org/10.1063/1.2218330.

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16

Friedman, B., T. A. Carter, M. V. Umansky, D. Schaffner, and I. Joseph. "Nonlinear instability in simulations of Large Plasma Device turbulence." Physics of Plasmas 20, no. 5 (2013): 055704. http://dx.doi.org/10.1063/1.4805084.

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17

TenBarge, J. M., G. G. Howes, W. Dorland, and G. W. Hammett. "An oscillating Langevin antenna for driving plasma turbulence simulations." Computer Physics Communications 185, no. 2 (2014): 578–89. http://dx.doi.org/10.1016/j.cpc.2013.10.022.

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18

Saini, Nadish, and Igor A. Bolotnov. "Two-Phase Turbulence Statistics from High Fidelity Dispersed Droplet Flow Simulations in a Pressurized Water Reactor (PWR) Sub-Channel with Mixing Vanes." Fluids 6, no. 2 (2021): 72. http://dx.doi.org/10.3390/fluids6020072.

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In the dispersed flow film boiling regime (DFFB), which exists under post-LOCA (loss-of-coolant accident) conditions in pressurized water reactors (PWRs), there is a complex interplay between droplet dynamics and turbulence in the surrounding steam. Experiments have accredited particular significance to droplet collision with the spacer-grids and mixing vane structures and their consequent positive feedback to the heat transfer recorded in the immediate downstream vicinity. Enabled by high-performance computing (HPC) systems and a massively parallel finite element-based flow solver—PHASTA (Par

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19

Meringolo, Claudio, Alejandro Cruz-Osorio, Luciano Rezzolla, and Sergio Servidio. "Microphysical Plasma Relations from Special-relativistic Turbulence." Astrophysical Journal 944, no. 2 (2023): 122. http://dx.doi.org/10.3847/1538-4357/acaefe.

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Abstract The microphysical, kinetic properties of astrophysical plasmas near accreting compact objects are still poorly understood. For instance, in modern general-relativistic magnetohydrodynamic simulations, the relation between the temperature of electrons T e and protons T p is prescribed in terms of simplified phenomenological models where the electron temperature is related to the proton temperature in terms of the ratio between the gas and magnetic pressures, or the β parameter. We here present a very comprehensive campaign of two-dimensional kinetic particle-in-cell simulations of spec

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20

Zhdankin, Vladimir. "Particle Energization in Relativistic Plasma Turbulence: Solenoidal versus Compressive Driving." Astrophysical Journal 922, no. 2 (2021): 172. http://dx.doi.org/10.3847/1538-4357/ac222e.

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Abstract Many high-energy astrophysical systems contain magnetized collisionless plasmas with relativistic particles, in which turbulence can be driven by an arbitrary mixture of solenoidal and compressive motions. For example, turbulence in hot accretion flows may be driven solenoidally by the magnetorotational instability or compressively by spiral shock waves. It is important to understand the role of the driving mechanism on kinetic turbulence and the associated particle energization. In this work, we compare particle-in-cell simulations of solenoidally driven turbulence with similar simul

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21

Vega, Cristian, Stanislav Boldyrev, and Vadim Roytershteyn. "Spectra of Magnetic Turbulence in a Relativistic Plasma." Astrophysical Journal Letters 931, no. 1 (2022): L10. http://dx.doi.org/10.3847/2041-8213/ac6cde.

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Abstract We present a phenomenological and numerical study of strong Alfvénic turbulence in a magnetically dominated collisionless relativistic plasma with a strong background magnetic field. In contrast with the nonrelativistic case, the energy in such turbulence is contained in magnetic and electric fluctuations. We argue that such turbulence is analogous to turbulence in a strongly magnetized nonrelativistic plasma in the regime of broken quasi-neutrality. Our 2D particle-in-cell numerical simulations of turbulence in a relativistic pair plasma find that the spectrum of the total energy has

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22

Vega, Cristian, Stanislav Boldyrev, and Vadim Roytershteyn. "Spatial Intermittency of Particle Distribution in Relativistic Plasma Turbulence." Astrophysical Journal 949, no. 2 (2023): 98. http://dx.doi.org/10.3847/1538-4357/accd73.

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Abstract Relativistic magnetically dominated turbulence is an efficient engine for particle acceleration in a collisionless plasma. Ultrarelativistic particles accelerated by interactions with turbulent fluctuations form nonthermal power-law distribution functions in the momentum (or energy) space, f(γ)d γ ∝ γ −α d γ, where γ is the Lorenz factor. We argue that in addition to exhibiting non-Gaussian distributions over energies, particles energized by relativistic turbulence also become highly intermittent in space. Based on particle-in-cell numerical simulations and phenomenological modeling,

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23

Meyrand, Romain, Anjor Kanekar, William Dorland, and Alexander A. Schekochihin. "Fluidization of collisionless plasma turbulence." Proceedings of the National Academy of Sciences 116, no. 4 (2019): 1185–94. http://dx.doi.org/10.1073/pnas.1813913116.

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In a collisionless, magnetized plasma, particles may stream freely along magnetic field lines, leading to “phase mixing” of their distribution function and consequently, to smoothing out of any “compressive” fluctuations (of density, pressure, etc.). This rapid mixing underlies Landau damping of these fluctuations in a quiescent plasma—one of the most fundamental physical phenomena that makes plasma different from a conventional fluid. Nevertheless, broad power law spectra of compressive fluctuations are observed in turbulent astrophysical plasmas (most vividly, in the solar wind) under condit

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24

Zheng, S. Y., D. B. Zhang, E. B. Xue та ін. "Study of turbulence in the high β _P discharge using only RF heating on EAST". Plasma Physics and Controlled Fusion 64, № 4 (2022): 045017. http://dx.doi.org/10.1088/1361-6587/ac4b07.

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Abstract High poloidal beta scenarios with a favorable energy confinement ( β p ∼ 1.9 , H 98 y 2 ∼ 1.4 ) have been achieved on the Experimental Advanced Superconducting Tokamak using only radio frequency wave heating. Gyrokinetic simulations are carried out with experimental plasma parameters and tokamak equilibrium data of a typical high β p discharge using the gyrokinetic toroidal code. Linear simulations show that electron-temperature scale length and electron-density scale length destabilize the turbulence, collision effects stabilize the turbulence, and the instability propagates in the e

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25

Oughton, S., W. H. Matthaeus, M. Wan, and K. T. Osman. "Anisotropy in solar wind plasma turbulence." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 373, no. 2041 (2015): 20140152. http://dx.doi.org/10.1098/rsta.2014.0152.

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A review of spectral anisotropy and variance anisotropy for solar wind fluctuations is given, with the discussion covering inertial range and dissipation range scales. For the inertial range, theory, simulations and observations are more or less in accord, in that fluctuation energy is found to be primarily in modes with quasi-perpendicular wavevectors (relative to a suitably defined mean magnetic field), and also that most of the fluctuation energy is in the vector components transverse to the mean field. Energy transfer in the parallel direction and the energy levels in the parallel componen

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26

Perrone, D., T. Passot, D. Laveder, et al. "Fluid simulations of plasma turbulence at ion scales: Comparison with Vlasov-Maxwell simulations." Physics of Plasmas 25, no. 5 (2018): 052302. http://dx.doi.org/10.1063/1.5026656.

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27

Hankla, Amelia M., Vladimir Zhdankin, Gregory R. Werner, Dmitri A. Uzdensky, and Mitchell C. Begelman. "Kinetic simulations of imbalanced turbulence in a relativistic plasma: Net flow and particle acceleration." Monthly Notices of the Royal Astronomical Society 509, no. 3 (2021): 3826–41. http://dx.doi.org/10.1093/mnras/stab3209.

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ABSTRACT Turbulent high-energy astrophysical systems often feature asymmetric energy injection: for instance, Alfvén waves propagating from an accretion disc into its corona. Such systems are ‘imbalanced’: the energy fluxes parallel and antiparallel to the large-scale magnetic field are unequal. In the past, numerical studies of imbalanced turbulence have focused on the magnetohydrodynamic regime. In this study, we investigate externally driven imbalanced turbulence in a collision-less, ultrarelativistically hot, magnetized pair plasma using 3D particle-in-cell (PIC) simulations. We find that

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28

Trotta, Domenico, Francesco Valentini, David Burgess, and Sergio Servidio. "Phase space transport in the interaction between shocks and plasma turbulence." Proceedings of the National Academy of Sciences 118, no. 21 (2021): e2026764118. http://dx.doi.org/10.1073/pnas.2026764118.

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The interaction of collisionless shocks with fully developed plasma turbulence is numerically investigated. Hybrid kinetic simulations, where a turbulent jet is slammed against an oblique shock, are employed to address the role of upstream turbulence on plasma transport. A technique, using coarse graining of the Vlasov equation, is proposed, showing that the particle transport strongly depends on upstream turbulence properties, such as strength and coherency. These results might be relevant for the understanding of acceleration and heating processes in space plasmas.

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29

Hellinger, Petr, Victor Montagud-Camps, Luca Franci, et al. "Ion-scale Transition of Plasma Turbulence: Pressure–Strain Effect." Astrophysical Journal 930, no. 1 (2022): 48. http://dx.doi.org/10.3847/1538-4357/ac5fad.

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Abstract We investigate properties of solar-wind-like plasma turbulence using direct numerical simulations. We analyze the transition from large, magnetohydrodynamic (MHD) scales to the ion characteristic ones using two-dimensional hybrid (fluid electrons and kinetic ions) simulations. To capture and quantify turbulence properties, we apply the Karman–Howarth–Monin (KHM) equation for compressible Hall–MHD (extended by considering the plasma pressure as a tensor quantity) to the numerical results. The KHM analysis indicates that the transition from MHD to ion scales (the so-called ion break in

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30

Papadopoulos, Aristeides D., Johan Anderson, Eun-jin Kim, Michail Mavridis, and Heinz Isliker. "Statistical Analysis of Plasma Dynamics in Gyrokinetic Simulations of Stellarator Turbulence." Entropy 25, no. 6 (2023): 942. http://dx.doi.org/10.3390/e25060942.

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A geometrical method for assessing stochastic processes in plasma turbulence is investigated in this study. The thermodynamic length methodology allows using a Riemannian metric on the phase space; thus, distances between thermodynamic states can be computed. It constitutes a geometric methodology to understand stochastic processes involved in, e.g., order–disorder transitions, where a sudden increase in distance is expected. We consider gyrokinetic simulations of ion-temperature-gradient (ITG)-mode-driven turbulence in the core region of the stellarator W7-X with realistic quasi-isodynamic to

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31

Lee, Sang-Yun, L. F. Ziebell, P. H. Yoon, R. Gaelzer, and E. S. Lee. "Particle-in-cell and Weak Turbulence Simulations of Plasma Emission." Astrophysical Journal 871, no. 1 (2019): 74. http://dx.doi.org/10.3847/1538-4357/aaf476.

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32

Bernard, T. N., E. L. Shi, K. W. Gentle, et al. "Gyrokinetic continuum simulations of plasma turbulence in the Texas Helimak." Physics of Plasmas 26, no. 4 (2019): 042301. http://dx.doi.org/10.1063/1.5085457.

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33

Fogaccia, G., R. Benzi, and F. Romanelli. "Lattice Boltzmann algorithm for three-dimensional simulations of plasma turbulence." Physical Review E 54, no. 4 (1996): 4384–93. http://dx.doi.org/10.1103/physreve.54.4384.

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34

Tang, William, Bei Wang, and Stephane Ethier. "Scientific Discovery in Fusion Plasma Turbulence Simulations at Extreme Scale." Computing in Science & Engineering 16, no. 5 (2014): 44–52. http://dx.doi.org/10.1109/mcse.2014.54.

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Thyagaraja, A. "Numerical simulations of tokamak plasma turbulence and internal transport barriers." Plasma Physics and Controlled Fusion 42, no. 12B (2000): B255—B269. http://dx.doi.org/10.1088/0741-3335/42/12b/320.

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36

Waltz, R. E., and R. L. Miller. "Ion temperature gradient turbulence simulations and plasma flux surface shape." Physics of Plasmas 6, no. 11 (1999): 4265–71. http://dx.doi.org/10.1063/1.873694.

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37

Ross, David W., and William Dorland. "Comparing simulation of plasma turbulence with experiment. II. Gyrokinetic simulations." Physics of Plasmas 9, no. 12 (2002): 5031–35. http://dx.doi.org/10.1063/1.1518997.

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38

Oppenheim, Meers M., and Yakov S. Dimant. "First 3-D simulations of meteor plasma dynamics and turbulence." Geophysical Research Letters 42, no. 3 (2015): 681–87. http://dx.doi.org/10.1002/2014gl062411.

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39

GHOSH, SHANKAR, and KRISHNAN MAHESH. "DNS of the thermal effects of laser energy deposition in isotropic turbulence." Journal of Fluid Mechanics 654 (May 14, 2010): 387–416. http://dx.doi.org/10.1017/s0022112010000649.

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The interaction of a laser-induced plasma with isotropic turbulence is studied using numerical simulations. The simulations use air as the working fluid and assume local thermodynamic equilibrium. The numerical method is fully spectral and uses a shock-capturing scheme in a corrector step. A model problem involving the effect of energy deposition on an isolated vortex is studied as a first step towards plasma/turbulence interaction. Turbulent Reynolds number Reλ = 30 and fluctuation Mach numbers Mt = 0.001 and 0.3 are considered. A tear-drop-shaped shock wave is observed to propagate into the

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Santos-Lima, R., G. Guerrero, E. M. de Gouveia Dal Pino, and A. Lazarian. "Diffusion of large-scale magnetic fields by reconnection in MHD turbulence." Monthly Notices of the Royal Astronomical Society 503, no. 1 (2021): 1290–309. http://dx.doi.org/10.1093/mnras/stab470.

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ABSTRACT The rate of magnetic field diffusion plays an essential role in several astrophysical plasma processes. It has been demonstrated that the omnipresent turbulence in astrophysical media induces fast magnetic reconnection, which consequently leads to large-scale magnetic flux diffusion at a rate independent of the plasma microphysics. This process is called 'reconnection diffusion' (RD) and allows for the diffusion of fields, which are dynamically important. The current theory describing RD is based on incompressible magnetohydrodynamic (MHD) turbulence. In this work, we have tested quan

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ELIASSON, BENGT. "FULL-SCALE SIMULATIONS OF IONOSPHERIC LANGMUIR TURBULENCE." Modern Physics Letters B 27, no. 08 (2013): 1330005. http://dx.doi.org/10.1142/s0217984913300056.

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This brief review is devoted to full-scale numerical modeling of the nonlinear interactions between electromagnetic (EM) waves and the ionosphere, giving rise to ionospheric Langmuir turbulence. A numerical challenge in the full-scale modeling is that it involves very different length- and time-scales. While the EM waves have wavelengths of the order 100 meters, the ionospheric Langmuir turbulence involving electrostatic waves and nonlinear structures can have wavelengths below one meter. A full-scale numerical scheme must resolve these different length- and time-scales, as well as the ionosph

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42

Dyrud, L. P., J. Urbina, J. T. Fentzke, E. Hibbit, and J. Hinrichs. "Global variation of meteor trail plasma turbulence." Annales Geophysicae 29, no. 12 (2011): 2277–86. http://dx.doi.org/10.5194/angeo-29-2277-2011.

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Abstract. We present the first global simulations on the occurrence of meteor trail plasma irregularities. These results seek to answer the following questions: when a meteoroid disintegrates in the atmosphere, will the resulting trail become plasma turbulent? What are the factors influencing the development of turbulence? and how do these trails vary on a global scale? Understanding meteor trail plasma turbulence is important because turbulent meteor trails are visible as non-specular trails to coherent radars. Turbulence also influences the evolution of specular radar meteor trails; this fac

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Vega, Cristian, Stanislav Boldyrev, and Vadim Roytershteyn. "Anisotropic Particle Acceleration in Alfvénic Turbulence." Astrophysical Journal 985, no. 2 (2025): 231. https://doi.org/10.3847/1538-4357/add147.

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Abstract Alfvénic turbulence is an effective mechanism for particle acceleration in strongly magnetized, relativistic plasma. In this study, we investigate a scenario where turbulent plasma is influenced by a strong guide magnetic field, resulting in highly anisotropic turbulent fluctuations. In such cases, the magnetic moments of particles are conserved, which means that acceleration can only occur along the direction of the magnetic field. Consistent with previous analytic studies, we find through particle-in-cell simulations of magnetically dominated pair plasma that the momenta of accelera

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44

Fulat, Karol, Artem Bohdan, Gabriel Torralba Paz, and Martin Pohl. "Kinetic Simulations of Nonrelativistic High-mach-number Perpendicular Shocks Propagating in a Turbulent Medium." Astrophysical Journal 959, no. 2 (2023): 119. http://dx.doi.org/10.3847/1538-4357/ad04dc.

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Abstract Strong nonrelativistic shocks are known to accelerate particles up to relativistic energies. However, for diffusive shock acceleration, electrons must have a highly suprathermal energy, implying the need for very efficient preacceleration. Most published studies consider shocks propagating through homogeneous plasma, which is an unrealistic assumption for astrophysical environments. Using 2D3V particle-in-cell simulations, we investigate electron acceleration and heating processes at nonrelativistic high-Mach-number shocks in electron-ion plasma with a turbulent upstream medium. For t

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Comişel, Horia, Yasuhiro Nariyuki, Yasuhito Narita, and Uwe Motschmann. "On the role of ion-scale whistler waves in space and astrophysical plasma turbulence." Annales Geophysicae 34, no. 11 (2016): 975–84. http://dx.doi.org/10.5194/angeo-34-975-2016.

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Abstract. Competition of linear mode waves is studied numerically to understand the energy cascade mechanism in plasma turbulence on ion-kinetic scales. Hybrid plasma simulations are performed in a 3-D simulation box by pumping large-scale Alfvén waves on the fluid scale. The result is compared with that from our earlier 2-D simulations. We find that the whistler mode is persistently present both in the 2-D and 3-D simulations irrespective of the initial setup, e.g., the amplitude of the initial pumping waves, while all the other modes are excited and damped such that the energy is efficiently

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Sisti, M., S. Fadanelli, S. S. Cerri, M. Faganello, F. Califano, and O. Agullo. "Characterizing current structures in 3D hybrid-kinetic simulations of plasma turbulence." Astronomy & Astrophysics 655 (November 2021): A107. http://dx.doi.org/10.1051/0004-6361/202141902.

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Context. In space and astrophysical plasmas, turbulence leads to the development of coherent structures characterized by a strong current density and important magnetic shears. Aims. Using hybrid-kinetic simulations of turbulence (3D with different energy injection scales), we investigate the development of these coherent structures and characterize their shape. Methods. First, we present different methods to estimate the overall shape of the 3D structure using local measurements, foreseeing an application on satellite data. Then we study the local magnetic configuration inside and outside cur

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Stepanenko, A. A. "Effects of magnetic geometry on dynamics of current-convective turbulence in tokamak divertor plasma." Physics of Plasmas 29, no. 12 (2022): 122309. http://dx.doi.org/10.1063/5.0119629.

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The current-convective instability is one of the physical mechanisms that can drive fluctuating transport of plasma in the tokamak divertor. The impact of the tokamak magnetic geometry on spatial and temporal properties of saturated turbulence, driven by the instability, is investigated. The analysis is performed by employing the basic model of the instability [A. A. Stepanenko and S. I. Krasheninnikov, Phys. Plasmas 25, 012305 (2018)] extended to include contributions from the interchange drive. Turbulence simulations are carried out in BOUT++ under DIII-D-like conditions. The dependencies of

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Bañón Navarro, A., A. Di Siena, J. L. Velasco, et al. "First-principles based plasma profile predictions for optimized stellarators." Nuclear Fusion 63, no. 5 (2023): 054003. http://dx.doi.org/10.1088/1741-4326/acc3af.

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Abstract In the present Letter, first-of-its-kind computer simulations predicting plasma profiles for modern optimized stellarators—while self-consistently retaining neoclassical transport, turbulent transport with 3D effects, and external physical sources—are presented. These simulations exploit a newly developed coupling framework involving the global gyrokinetic turbulence code GENE-3D, the neoclassical transport code KNOSOS, and the 1D transport solver TANGO. This framework is used to analyze the recently observed degradation of energy confinement in electron-heated plasmas in the Wendelst

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Ricketson, L., A. Hakim, and J. Hittinger. "Consistent coupling algorithms for coupled core-edge simulations of plasma turbulence." Physics of Plasmas 28, no. 1 (2021): 012301. http://dx.doi.org/10.1063/5.0027670.

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Franci, Luca, Simone Landi, Lorenzo Matteini, Andrea Verdini, and Petr Hellinger. "HIGH-RESOLUTION HYBRID SIMULATIONS OF KINETIC PLASMA TURBULENCE AT PROTON SCALES." Astrophysical Journal 812, no. 1 (2015): 21. http://dx.doi.org/10.1088/0004-637x/812/1/21.

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