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Journal articles on the topic 'Simulations HPC de plasma turbulent'

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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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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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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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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5

Baudoin, Camille, Patrick Tamain, Hugo Bufferand, et al. "Turbulent heat transport in TOKAM3X edge plasma simulations." Contributions to Plasma Physics 58, no. 6-8 (2018): 484–89. http://dx.doi.org/10.1002/ctpp.201700168.

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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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Nunami, M., S. Toda, M. Nakata, and H. Sugama. "Improved prediction scheme for ion heat turbulent transport." Physics of Plasmas 29, no. 10 (2022): 102505. http://dx.doi.org/10.1063/5.0103447.

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A novel scheme to predict the turbulent transport of ion heat of magnetic confined plasmas is developed by combining mathematical optimization techniques employed in data analysis approaches and first-principle gyrokinetic simulations. Gyrokinetic simulation, as a first-principle approach, is a reliable way to predict turbulent transport. However, in terms of the flux-matching [Candy et al., Phys. Plasmas 16, 060704 (2009)], quantitative transport estimates by gyrokinetic simulations incur extremely heavy computational costs. In order to reduce the costs of quantitative transport prediction ba

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8

Gleize, Vincent, Michel Costes, and Ivan Mary. "Numerical simulation of NACA4412 airfoil in pre-stall conditions." International Journal of Numerical Methods for Heat & Fluid Flow 32, no. 4 (2021): 1375–97. http://dx.doi.org/10.1108/hff-07-2021-0514.

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Purpose The purpose of this paper is to study turbulent flow separation at the airfoil trailing edge. This work aims to improve the knowledge of stall phenomenon by creating a QDNS database for the NACA412 airfoil. Design/methodology/approach Quasi-DNS simulations of the NACA 4412 airfoil in pre-stall conditions have been completed. The Reynolds number based on airfoil chord and freestream velocity is equal to 0.35 million, and the freestream Mach number to 0.117. Transition is triggered on both surfaces for avoiding the occurrence of laminar separation bubbles and to ensure turbulent mixing i

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9

Rincon, François, Francesco Califano, Alexander A. Schekochihin, and Francesco Valentini. "Turbulent dynamo in a collisionless plasma." Proceedings of the National Academy of Sciences 113, no. 15 (2016): 3950–53. http://dx.doi.org/10.1073/pnas.1525194113.

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Magnetic fields pervade the entire universe and affect the formation and evolution of astrophysical systems from cosmological to planetary scales. The generation and dynamical amplification of extragalactic magnetic fields through cosmic times (up to microgauss levels reported in nearby galaxy clusters, near equipartition with kinetic energy of plasma motions, and on scales of at least tens of kiloparsecs) are major puzzles largely unconstrained by observations. A dynamo effect converting kinetic flow energy into magnetic energy is often invoked in that context; however, extragalactic plasmas

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10

Kitiashvili, I. N., A. G. Kosovichev, A. A. Wray, and N. N. Mansour. "Realistic MHD simulations of magnetic self-organization in solar plasma." Proceedings of the International Astronomical Union 6, S274 (2010): 120–24. http://dx.doi.org/10.1017/s1743921311006703.

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AbstractFilamentary structure is a fundamental property of the magnetized solar plasma. Recent high-resolution observations and numerical simulations have revealed close links between the filamentary structures and plasma dynamics in large-scale solar phenomena, such as sunspots and magnetic network. A new emerging paradigm is that the mechanisms of the filamentary structuring and large-scale organization are natural consequences of turbulent magnetoconvection on the Sun. We present results of 3D radiative MHD large-eddy simulations (LES) of magnetic structures in the turbulent convective boun

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Timofeev, I. V., and A. V. Terekhov. "Simulations of turbulent plasma heating by powerful electron beams." Physics of Plasmas 17, no. 8 (2010): 083111. http://dx.doi.org/10.1063/1.3474952.

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12

Timofeev, I. V., and A. V. Terekhov. "Simulations of Turbulent Plasma Heating by Powerful Electron Beams." Fusion Science and Technology 59, no. 1T (2011): 70–73. http://dx.doi.org/10.13182/fst11-a11577.

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13

Pucci, F., M. Viviani, F. Valentini, G. Lapenta, W. H. Matthaeus, and S. Servidio. "Turbulent Magnetogenesis in a Collisionless Plasma." Astrophysical Journal Letters 922, no. 1 (2021): L18. http://dx.doi.org/10.3847/2041-8213/ac36cf.

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Abstract We demonstrate an efficient mechanism for generating magnetic fields in turbulent, collisionless plasmas. By using fully kinetic, particle-in-cell simulations of an initially nonmagnetized plasma, we inspect the genesis of magnetization, in a nonlinear regime. The complex motion is initiated via a Taylor–Green vortex, and the plasma locally develops strong electron temperature anisotropy, due to the strain tensor of the turbulent flow. Subsequently, in a domino effect, the anisotropy triggers a Weibel instability, localized in space. In such active wave–particle interaction regions, t

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Oyarzun, Guillermo, and Athanassios Dimas. "TURBULENT OSCILLATORY FLOW OVER RIPPLES AT HIGH REYNOLDS NUMBERS FOR PETA-SCALE SIMULATIONS." Coastal Engineering Proceedings, no. 36 (December 30, 2018): 95. http://dx.doi.org/10.9753/icce.v36.sediment.95.

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Surface waves in the coastal zone induce oscillatory flow motions in the vicinity of the seabed. These wave-induced coastal flows interact with the sandy seabed and modify the bed shape by generating coherent small-scale bed structures, which are generally known as ripples. The presence of ripples in oscillatory flows is important due to the impact they have on the seabed roughness and how they affect the near-bed boundary layer hydrodynamics. Simulations of higher and more real-scale Reynolds number (Re) require the use of supercomputers in order to obtain results in a reasonable amount of ti

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SHAIKH, DASTGEER, and G. P. ZANK. "Turbulent spectra in the solar wind plasma." Journal of Plasma Physics 76, no. 2 (2009): 183–91. http://dx.doi.org/10.1017/s0022377809990237.

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AbstractObservations of interstellar scintillations at radio wavelengths reveal a Kolmogorov-like scaling of the electron density spectrum with a spectral slope of −5/3 over six decades in wavenumber space. A similar turbulent density spectrum in the solar wind plasma has been reported. The energy transfer process in the magnetized solar wind plasma over such extended length scales remains an unresolved paradox of modern turbulence theories, raising the especially intriguing question of how a compressible magnetized solar wind exhibits a turbulent spectrum that is a characteristic of an incomp

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Thévenin, Sébastien, Nicolas Valade, Benoît-Joseph Gréa, Gilles Kluth, and Olivier Soulard. "Modeling compressed turbulent plasma with rapid viscosity variations." Physics of Plasmas 29, no. 11 (2022): 112310. http://dx.doi.org/10.1063/5.0115272.

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We propose two-equation models in order to capture the dynamics of a turbulent plasma undergoing compression and experiencing large viscosity variations. The models account for possible relaminarization phases and rapid viscosity changes through closures dependent on the turbulent Reynolds and on the viscosity Froude numbers. These closures are determined from a data-driven approach using eddy-damped quasi-normal Markovian simulations. The best model is able to mimic the various self-similar regimes identified in Viciconte et al. [Phys. Rev. E 97, 023201 (1998)] and to recover the rapid transi

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17

NISHIKAWA, K. I., J. NIMIEC, M. MEDVEDEV, et al. "RADIATION FROM RELATIVISTIC SHOCKS WITH TURBULENT MAGNETIC FIELDS." International Journal of Modern Physics D 19, no. 06 (2010): 715–21. http://dx.doi.org/10.1142/s0218271810016865.

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Using our new 3D relativistic electromagnetic particle (REMP) code parallelized with MPI, we investigated long-term particle acceleration associated with a relativistic electron–positron jet propagating in an unmagnetized ambient electron–positron plasma. We have also performed simulations with electron-ion jets. The simulations were performed using a much longer simulation system than our previous simulations in order to investigate the full nonlinear stage of the Weibel instability for electron–positron jets and its particle acceleration mechanism. Cold jet electrons are thermalized and ambi

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18

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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19

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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20

Theilhaber, K., G. Laval, and D. Pesme. "Numerical simulations of turbulent trapping in the weak beam–plasma instability." Physics of Fluids 30, no. 10 (1987): 3129. http://dx.doi.org/10.1063/1.866488.

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21

Reynolds-Barredo, J. M., D. E. Newman, R. Sanchez, D. Samaddar, L. A. Berry, and W. R. Elwasif. "Mechanisms for the convergence of time-parallelized, parareal turbulent plasma simulations." Journal of Computational Physics 231, no. 23 (2012): 7851–67. http://dx.doi.org/10.1016/j.jcp.2012.07.028.

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22

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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23

Bott, A. F. A., L. Chen, P. Tzeferacos, et al. "Insensitivity of a turbulent laser-plasma dynamo to initial conditions." Matter and Radiation at Extremes 7, no. 4 (2022): 046901. http://dx.doi.org/10.1063/5.0084345.

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It has recently been demonstrated experimentally that a turbulent plasma created by the collision of two inhomogeneous, asymmetric, weakly magnetized, laser-produced plasma jets can generate strong stochastic magnetic fields via the small-scale turbulent dynamo mechanism, provided the magnetic Reynolds number of the plasma is sufficiently large. In this paper, we compare such a plasma with one arising from two pre-magnetized plasma jets whose creation is identical save for the addition of a strong external magnetic field imposed by a pulsed magnetic field generator. We investigate the differen

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da Silva, F., E. Ricardo, J. Ferreira, et al. "Benchmarking 2D against 3D FDTD codes for the assessment of the measurement performance of a low field side plasma position reflectometer applicable to IDTT." Journal of Instrumentation 17, no. 01 (2022): C01017. http://dx.doi.org/10.1088/1748-0221/17/01/c01017.

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Abstract O-mode reflectometry, a technique to diagnose fusion plasmas, is foreseen as a source of real-time (RT) plasma position and shape measurements for control purposes in the coming generation of machines such as DEMO. It is, thus, of paramount importance to predict the behavior and capabilities of these new reflectometry systems using synthetic diagnostics. Finite-difference time-domain (FDTD) time-dependent codes allow for a comprehensive description of reflectometry but are computationally demanding, especially when it comes to three-dimensional (3D) simulations, which requires access

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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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Yang, Yan, Francesco Pecora, William H. Matthaeus, et al. "Quantifying the Agyrotropy of Proton and Electron Heating in Turbulent Plasmas." Astrophysical Journal 944, no. 2 (2023): 148. http://dx.doi.org/10.3847/1538-4357/acb25a.

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Abstract An important aspect of energy dissipation in weakly collisional plasmas is that of energy partitioning between different species (e.g., protons and electrons) and between different energy channels. Here we analyse pressure–strain interaction to quantify the fractions of isotropic compressive, gyrotropic, and nongyrotropic heating for each species. An analysis of kinetic turbulence simulations is compared and contrasted with corresponding observational results from Magnetospheric Multiscale Mission data in the magnetosheath. In assessing how protons and electrons respond to different i

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Arró, G., F. Califano, and G. Lapenta. "Statistical properties of turbulent fluctuations associated with electron-only magnetic reconnection." Astronomy & Astrophysics 642 (October 2020): A45. http://dx.doi.org/10.1051/0004-6361/202038696.

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Context. Recent satellite measurements in the turbulent magnetosheath of Earth have given evidence of an unusual reconnection mechanism that is driven exclusively by electrons. This newly observed process was called electron-only reconnection, and its interplay with plasma turbulence is a matter of great debate. Aims. By using 2D-3V hybrid Vlasov–Maxwell simulations of freely decaying plasma turbulence, we study the role of electron-only reconnection in the development of plasma turbulence. In particular, we search for possible differences with respect to the turbulence associated with standar

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Asai, N., N. Fukuda, and R. Matsumoto. "Three-Dimensional MHD Simulations of a Subcluster Plasma Moving in Turbulent ICM." Proceedings of the International Astronomical Union 2, S235 (2006): 189. http://dx.doi.org/10.1017/s1743921306005953.

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AbstractWe carried out 3D magnetohydrodynamic simulations of a subcluster moving in turbulent ICM by including anisotropic heat conduction. Since magnetic fields stretched along the subcluster surface suppress the heat conduction across the front, cold fronts are formed and sustained.

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Trotta, Domenico, Francesco Pecora, Adriana Settino, et al. "On the Transmission of Turbulent Structures across the Earth’s Bow Shock." Astrophysical Journal 933, no. 2 (2022): 167. http://dx.doi.org/10.3847/1538-4357/ac7798.

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Abstract Collisionless shocks and plasma turbulence are crucial ingredients for a broad range of astrophysical systems. The shock–turbulence interaction, and in particular the transmission of fully developed turbulence across the quasi-perpendicular Earth’s bow shock, is here addressed using a combination of spacecraft observations and local numerical simulations. An alignment between the Wind (upstream) and Magnetospheric Multiscale (downstream) spacecraft is used to study the transmission of turbulent structures across the shock, revealing an increase of their magnetic helicity content in it

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Acosta, Belén, Denisse Pastén, and Pablo S. Moya. "Reversibility of Turbulent and Non-Collisional Plasmas: Solar Wind." Proceedings of the International Astronomical Union 15, S354 (2019): 363–66. http://dx.doi.org/10.1017/s1743921320000137.

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AbstractWe have studied turbulent plasma as a complex system applying the method known as Horizontal Visibility Graph (HVG) to obtain the Kullback-Leibler Divergence (KLD) as a first approach to characterize the reversibility of the time series of the magnetic fluctuations. For this, we have developed the method on Particle In Cell (PIC) simulations for a magnetized plasma and on solar wind magnetic time series, considering slow and fast wind. Our numerical results show that low irreversibility values are verified for magnetic field time series associated with Maxwellian distributions. In addi

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Hasan, Mahdi, and Michael Atkinson. "Investigation of a Dielectric Barrier Discharge Plasma Actuator to Control Turbulent Boundary Layer Separation." Applied Sciences 10, no. 6 (2020): 1911. http://dx.doi.org/10.3390/app10061911.

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A numerical investigation was carried out to explore the effects of a dielectric barrier discharge (DBD) plasma actuator on a three-dimensional incompressible, separated flow. The test article selected for the simulations was the National Aeronautical and Space Administration (NASA) wall-mounted hump model. The simulations were run at a Reynolds number of 936,000, based on hump chord length, and a freestream Mach number of 0.1. Hybrid partially averaged Navier–Stokes/large-eddy simulations (PANS/LES) were completed using CALC-LES, a well-validated computational fluid dynamics (CFD) code, devel

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Bhide, Kalyani, Kiran Siddappaji, Shaaban Abdallah, and Kurt Roberts. "Improved Supersonic Turbulent Flow Characteristics Using Non-Linear Eddy Viscosity Relation in RANS and HPC-Enabled LES." Aerospace 8, no. 11 (2021): 352. http://dx.doi.org/10.3390/aerospace8110352.

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A majority of the eddy viscosity models for supersonic turbulent flow are based on linear relationship between Reynolds stresses and mean strain rate. The validity of these models can be improved by introducing non-linearity in relation as RANS models offer advantages in terms of reduced turnaround times typical of industry applications. With these benefits, the present work utilizes quadratic constitutive relation (QCR) with Menter’s k omega SST model to characterize the flowfield of rectangular jets. The sensitivity of this model with QCR, weighted towards diffusion, dissipation, and a combi

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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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Keskinen, M. J. "Theory of Strongly Turbulent Two-Dimensional Cross Field Convection of Current Carrying Space Plasmas." Symposium - International Astronomical Union 107 (1985): 475. http://dx.doi.org/10.1017/s0074180900075963.

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The “direct interaction approximation” of Kraichnan as modified by Kadomtsev is employed to develop a two-dimensional strong turbulence theory which predicts both nonlinear frequency broadening and a power law for the spectrum of a convecting plasma containing a gravitationally induced cross field current. These results are favorably compared with experimental observations, numerical simulations, and previous studies1 of turbulent cross field convection of current-carrying plasma.

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Bott, Archie F. A., Petros Tzeferacos, Laura Chen, et al. "Time-resolved turbulent dynamo in a laser plasma." Proceedings of the National Academy of Sciences 118, no. 11 (2021): e2015729118. http://dx.doi.org/10.1073/pnas.2015729118.

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Understanding magnetic-field generation and amplification in turbulent plasma is essential to account for observations of magnetic fields in the universe. A theoretical framework attributing the origin and sustainment of these fields to the so-called fluctuation dynamo was recently validated by experiments on laser facilities in low-magnetic-Prandtl-number plasmas (Pm<1). However, the same framework proposes that the fluctuation dynamo should operate differently when Pm≳1, the regime relevant to many astrophysical environments such as the intracluster medium of galaxy clusters. This paper r

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Shaikh, D., and G. P. Zank. "Three-dimensional simulations of turbulent spectra in the local interstellar medium." Nonlinear Processes in Geophysics 14, no. 4 (2007): 351–59. http://dx.doi.org/10.5194/npg-14-351-2007.

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Abstract. Three-dimensional time dependent numerical simulations of compressible magnetohydrodynamic fluids describing super-Alfvénic, supersonic and strongly magnetized space and laboratory plasmas show a nonlinear relaxation towards a state of near incompressibility. The latter is characterized essentially by a subsonic turbulent Mach number. This transition is mediated dynamically by disparate spectral energy dissipation rates in compressible magnetosonic and shear Alfvénic modes. Nonlinear cascades lead to super-Alfvénic turbulent motions decaying to a sub-Alfvénic regime that couples weak

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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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Bustard, Chad, and S. Peng Oh. "Turbulent Reacceleration of Streaming Cosmic Rays." Astrophysical Journal 941, no. 1 (2022): 65. http://dx.doi.org/10.3847/1538-4357/aca021.

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Abstract Subsonic, compressive turbulence transfers energy to cosmic rays (CRs), a process known as nonresonant reacceleration. It is often invoked to explain the observed ratios of primary to secondary CRs at ∼GeV energies, assuming wholly diffusive CR transport. However, such estimates ignore the impact of CR self-confinement and streaming. We study these issues in stirring box magnetohydrodynamic (MHD) simulations using Athena++, with field-aligned diffusive and streaming CR transport. For diffusion only, we find CR reacceleration rates in good agreement with analytic predictions. When stre

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Carlevaro, Nakia, Giovanni Montani, and Fabio Moretti. "On the Effects of Tokamak Plasma Edge Symmetries on Turbulence Relaxation." Symmetry 15, no. 9 (2023): 1745. http://dx.doi.org/10.3390/sym15091745.

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The plasma edge of a tokamak configuration is characterized by turbulent dynamics leading to enhanced transport. We construct a simplified 3D Hasegawa–Wakatani model reducing to a single partial differential equation for the turbulent electric potential dynamics. Simulations demonstrate how the 3D turbulence relaxes on a 2D axisymmetric profile, corresponding to the so-called interchange turbulence. The spectral features of this regime are found to be strongly dependent on the initialization pattern. We outline that the emergence of axisymmetric turbulence is also achieved when the correspondi

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WIECHEN, HEINZ M. "Simulations of Kelvin–Helmholtz modes in the dusty plasma environment of noctilucent clouds." Journal of Plasma Physics 73, no. 5 (2007): 649–58. http://dx.doi.org/10.1017/s0022377806006088.

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AbstractWe present results of quantitative multi-fluid simulations of the nonlinear dynamics of Kelvin–Helmholtz modes in the partially ionized dusty plasma of noctilucent clouds. Noctilucent clouds are a typical example of dusty plasmas in the Earth's mesosphere/lower thermosphere. A specific feature observed in noctilucent clouds is wavy, turbulent structure. Possible explanations for these structures, which are discussed in the literature, are based on hydrodynamical models. The dusty plasma aspect has been widely neglected, so far. In this paper we examine the nonlinear dynamics of Kelvin–

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Tamain, P., Ph Ghendrih, H. Bufferand, et al. "Multi-scale self-organisation of edge plasma turbulent transport in 3D global simulations." Plasma Physics and Controlled Fusion 57, no. 5 (2015): 054014. http://dx.doi.org/10.1088/0741-3335/57/5/054014.

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Blanchard, Victorien P., Yacine Bechane, Nicolas Q. Minesi, Stéphane Q. E. Wang, Benoît Fiorina, and Christophe O. Laux. "Experimental characterization and 3D simulations of turbulent flames assisted by nanosecond plasma discharges." Combustion and Flame 270 (December 2024): 113709. http://dx.doi.org/10.1016/j.combustflame.2024.113709.

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Yelles Chaouche, L., R. H. Cameron, S. K. Solanki, et al. "Power spectrum of turbulent convection in the solar photosphere." Astronomy & Astrophysics 644 (November 30, 2020): A44. http://dx.doi.org/10.1051/0004-6361/202037545.

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The solar photosphere provides us with a laboratory for understanding turbulence in a layer where the fundamental processes of transport vary rapidly and a strongly superadiabatic region lies very closely to a subadiabatic layer. Our tools for probing the turbulence are high-resolution spectropolarimetric observations such as have recently been obtained with the two balloon-borne SUNRISE missions, and numerical simulations. Our aim is to study photospheric turbulence with the help of Fourier power spectra that we compute from observations and simulations. We also attempt to explain some proper

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Ghanbari, Keyvan, and Vladimir Florinski. "Simulation of Solar Wind Turbulence near Corotating Interaction Regions: Superposed Epoch Analysis of Simulations and Observations." Astrophysical Journal 943, no. 2 (2023): 87. http://dx.doi.org/10.3847/1538-4357/acabc4.

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Abstract The effect of the turbulence that is associated with solar wind corotating interaction regions (CIRs) on transport of galactic cosmic rays remains an outstanding problem in space science. Observations show that the intensities of the plasma and magnetic fluctuations are enhanced within a CIR. The velocity shear layer between the slow and fast wind embedded in a CIR is thought to be responsible for this enhancement in turbulent energy. We perform physics-based magnetohydrodynamic simulations of the plasma background and turbulent fluctuations in the solar wind dominated by CIRs for rad

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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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Yeates, A. R., A. J. B. Russell, and G. Hornig. "Physical role of topological constraints in localized magnetic relaxation." Proceedings of the Royal Society A: Mathematical, Physical and Engineering Sciences 471, no. 2178 (2015): 20150012. http://dx.doi.org/10.1098/rspa.2015.0012.

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Predicting the final state of turbulent plasma relaxation is an important challenge, both in astro-physical plasmas such as the Sun's corona and in controlled thermonuclear fusion. Recent numerical simulations of plasma relaxation with braided magnetic fields identified the possibility of a novel constraint, arising from the topological degree of the magnetic field-line mapping. This constraint implies that the final relaxed state is drastically different for an initial configuration with topological degree 1 (which allows a Taylor relaxation) and one with degree 2 (which does not reach a Tayl

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Xiong, Q. Y., Tulasi N. Parashar, S. Y. Huang, et al. "Effects of Alpha Particle Fraction on Kinetic Plasma Turbulence." Astrophysical Journal 968, no. 2 (2024): 93. http://dx.doi.org/10.3847/1538-4357/ad4643.

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Abstract Solar activities have an extraordinary impact on interplanetary space, enriching the plasma dynamics including turbulent heating of various species. The small fraction of alpha particles is believed to play a significant role in the turbulent dynamics of the solar wind. Here we present fully kinetic particle-in-cell simulations to reveal the influences of the alpha particles in decaying plasma turbulence. Multiple run cases with different controlled variations of proton and alpha density are performed to compare and evaluate the energy conversion processes. It is found that the alpha

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Park, Kiwan. "α Effect and Magnetic Diffusivity β in Helical Plasma Under Turbulence Growth". Universe 11, № 7 (2025): 203. https://doi.org/10.3390/universe11070203.

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We investigate the transport coefficients α and β in plasma systems with varying Reynolds numbers while maintaining a unit magnetic Prandtl number (PrM). The α and β tensors parameterize the turbulent electromotive force (EMF) in terms of the large-scale magnetic field B¯ and current density as follows: ⟨u×b⟩=αB¯−β∇×B¯. In astrophysical plasmas, high fluid Reynolds numbers (Re) and magnetic Reynolds numbers (ReM) drive turbulence, where Re governs flow dynamics and ReM controls magnetic field evolution. The coefficients αsemi and βsemi are obtained from large-scale magnetic field data as estim

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Casner, A., G. Rigon, B. Albertazzi, et al. "Turbulent hydrodynamics experiments in high energy density plasmas: scientific case and preliminary results of the TurboHEDP project." High Power Laser Science and Engineering 6 (2018). http://dx.doi.org/10.1017/hpl.2018.34.

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The physics of compressible turbulence in high energy density (HED) plasmas is an unchartered experimental area. Simulations of compressible and radiative flows relevant for astrophysics rely mainly on subscale parameters. Therefore, we plan to perform turbulent hydrodynamics experiments in HED plasmas (TurboHEDP) in order to improve our understanding of such important phenomena for interest in both communities: laser plasma physics and astrophysics. We will focus on the physics of supernovae remnants which are complex structures subject to fluid instabilities such as the Rayleigh–Taylor and K

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Coosemans, Reinart, Wouter Dekeyser, and Martine Baelmans. "Mean-field transport equations and energy theorem for plasma edge turbulent transport." Journal of Plasma Physics 90, no. 2 (2024). http://dx.doi.org/10.1017/s0022377824000163.

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This paper establishes a mean-field equation set and an energy theorem to provide a theoretical basis in view of the development of self-consistent, physics-based turbulent transport models for mean-field transport codes. A rigorous averaging procedure identifies the exact form of the perpendicular turbulent fluxes which are modelled by ad hoc diffusive terms in mean-field transport codes, next to other closure terms which are not commonly considered. Earlier work suggested that the turbulent $E\times B$ particle and heat fluxes, which are thus identified to be important closure terms, can be

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