Scale Separation Effects on Simulations of Plasma Turbulence

• Published in: The Astrophysical journal Vol. 972; no. 2; pp. 173 - 184
• Main Authors: Edyvean, Jago, Parashar, Tulasi N., Simpson, Tom, Juno, James, Delzanno, Gian Luca, Guo, Fan, Koshkarov, Oleksandr, Matthaeus, William H, Shay, Michael, Yang, Yan
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01-09-2024; IOP Publishing
• Subjects: Asymptotic properties; Dissipation; Electron heating; Electron mass; Electrons; Fluid flow; Heating; Incompressible flow; Interplanetary turbulence; Ions; Light speed; Numerical experiments; Plasma astrophysics; Plasma physics; Plasma turbulence; Solar wind; Space plasmas; Viscosity
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad5cf5

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 taken to use values as close as possible to realistic values within the computational constraints, these artificial values could potentially introduce unphysical effects. These unphysical effects could be significant at sub-ion scales, where kinetic effects are the most important. In this paper, we use the 10-moment fluid model in the Gkeyll framework to perform controlled numerical experiments, systematically varying the ion–electron mass ratio from a small value down to the realistic proton–electron mass ratio. We show that the unphysical mass ratio has a significant effect on the kinetic range dynamics as well as the heating of both plasma species. The dissipative process for both ions and electrons becomes more compressive in nature, although the ions remain nearly incompressible in all cases. The electrons move from being dominated by incompressive viscous-like heating/dissipation to very compressive heating/dissipation dominated by compressions/rarefactions. While the heating change is significant for the electrons, a mass ratio of m i / m e ∼ 250 captures the asymptotic behavior of electron heating.