ABSTRACT Intermittency of heating in weakly collisional plasma turbulence is an active subject of research, with significant potential impact on understanding of the solar wind, solar corona, and ...astrophysical plasmas. Recent studies suggest a role of vorticity in plasma heating. In magnetohydrodynamics small-scale vorticity is generated near current sheets and this effect persists in kinetic plasma, as demonstrated here with hybrid and fully kinetic particle-in-cell simulations. Furthermore, vorticity enhances local kinetic effects, with a generalized resonance condition selecting sign-dependent enhancements or reductions of proton heating and thermal anisotropy. In such plasmas heating is correlated with vorticity and current density, but more strongly with vorticity. These results help explain several prior results that find kinetic effects and energization near to, but not centered on, current sheets. Evidently intermittency in kinetic plasma involves multiple physical quantities, and the associated coherent structures and nonthermal effects are closely related.
Plasma turbulence is investigated using unprecedented high-resolution ion velocity distribution measurements by the Magnetospheric Multiscale mission (MMS) in the Earth's magnetosheath. This novel ...observation of a highly structured particle distribution suggests a cascadelike process in velocity space. Complex velocity space structure is investigated using a three-dimensional Hermite transform, revealing, for the first time in observational data, a power-law distribution of moments. In analogy to hydrodynamics, a Kolmogorov approach leads directly to a range of predictions for this phase-space transport. The scaling theory is found to be in agreement with observations. The combined use of state-of-the-art MMS data sets, novel implementation of a Hermite transform method, and scaling theory of the velocity cascade opens new pathways to the understanding of plasma turbulence and the crucial velocity space features that lead to dissipation in plasmas.
Full text
Available for:
CMK, CTK, FMFMET, IJS, NUK, PNG, UM
What is the Reynolds Number of the Solar Wind? Wrench, Daniel; Parashar, Tulasi N.; Oughton, Sean ...
Astrophysical journal/The Astrophysical journal,
02/2024, Volume:
961, Issue:
2
Journal Article
Peer reviewed
Open access
Abstract
The Reynolds number,
Re
, is an important quantity for describing a turbulent flow. It tells us about the bandwidth over which energy can cascade from large scales to smaller ones, prior to ...the onset of dissipation. However, calculating it for nearly collisionless plasmas like the solar wind is challenging. Previous studies have used formulations of an “effective” Reynolds number, expressing
Re
as a function of the correlation scale and either the Taylor scale or a proxy for the dissipation scale. We find that the Taylor scale definition of the Reynolds number has a sizable prefactor of approximately 27, which has not been employed in previous works. Drawing from 18 years of data from the Wind spacecraft at 1 au, we calculate the magnetic Taylor scale directly and use both the ion inertial length and the magnetic spectrum break scale as approximations for the dissipation scale, yielding three distinct
Re
estimates for each 12 hr interval. Average values of
Re
range between 116,000 and 3,406,000 within the general distribution of past work. We also find considerable disagreement between the methods, with linear associations of between 0.38 and 0.72. Although the Taylor scale method is arguably more physically motivated, due to its dependence on the energy cascade rate, more theoretical work is needed in order to identify the most appropriate way of calculating effective Reynolds numbers for kinetic plasmas. As a summary of our observational analysis, we make available a data product of 28 years of 1 au solar wind and magnetospheric plasma measurements from Wind.
Two-and-one-half dimensional particle-in-cell simulations of the forward cascade and dissipation of decaying kinetic Alfvénic turbulence have been carried out on a model of a collisionless, ...homogeneous, magnetized ion-electron plasma. The uniform background magnetic field o lies parallel to the simulation plane. The simulations were executed as part of the Turbulent Dissipation Challenge. Initial narrowband magnetic fluctuation spectra of kinetic range Alfvén waves undergo a forward cascade to broadband turbulent spectra at shorter wavelengths, at the same time undergoing dissipative transfer of fluctuating field energy to kinetic energy of electrons and ions. The simulations yield Qi and Qe, the dimensionless rates of kinetic energy density gain for ions (subscript i) and electrons (subscript e). These are computed for five different initial values of βi/βe. For the parameters chosen here, the simulations yield the scaling relation Qe/Qi 2(Ti/Te)2 where Tj represents the initial temperature of the jth species. For all simulation times the kinetic anisotropy of the ions changes monotonically in the sense of greater energy passing from the fluctuations into ion velocities parallel to, rather than perpendicular to, o, suggesting that Landau damping is an important ion dissipation mechanism for kinetic Alfvénic turbulence.
ABSTRACT Analysis of particle-in-cell simulations of kinetic plasma turbulence reveals a connection between the strength of cascade, the total heating rate, and the partitioning of dissipated energy ...into proton heating and electron heating. A von Karman scaling of the cascade rate explains the total heating across several families of simulations. The proton to electron heating ratio increases in proportion to total heating. We argue that the ratio of gyroperiod to nonlinear turnover time at the ion kinetic scales controls the ratio of proton and electron heating. The proposed scaling is consistent with simulations.
Abstract
Alfvénicity is a well-known property, common in the solar wind, characterized by a high correlation between magnetic and velocity fluctuations. Data from the Parker Solar Probe (PSP) enable ...the study of this property closer to the Sun than ever before, as well as in the sub-Alfvénic solar wind. We consider scale-dependent measures of Alfvénicity based on second-order functions of the magnetic and velocity increments as a function of time lag, including the normalized cross helicity
σ
c
and residual energy
σ
r
. Scale-dependent Alfvénicity is strongest for lags near the correlation scale and increases when moving closer to the Sun. We find that
σ
r
typically remains close to the maximally negative value compatible with
σ
c
. We did not observe significant changes in measures of Alfvénicity between sub-Alfvénic and super-Alfvénic wind. During most times, the solar wind was highly Alfvénic; however, lower Alfvénicity was observed when PSP approached the heliospheric current sheet or other magnetic structures with sudden changes in the radial magnetic field, non-unidirectional strahl electron pitch angle distributions, and strong electron density contrasts. These results are consistent with a picture in which Alfvénic fluctuations generated near the photosphere transport outward, forming highly Alfvénic states in the young solar wind, and subsequent interactions with large-scale structures and gradients lead to weaker Alfvénicity, as commonly observed at larger heliocentric distances.
PDF
