Low alpha temperatures in the solar wind magnetic closed structures

Summary As is already known, closed structures in interplanetary magnetic field reduce the solar-wind electron and proton temperatures and possibly diminish the flux of low-rigidity cosmic rays within them. In this analysis, an attempt is made to search for any influence of closed structures on the alpha component,i.e. to detect a possible cooling and rarefaction of these ions like protons, when they are encircled by these structures. Seven isolated events of such features are used for a superposed epoch analysis from a 5-year period data set provided by Helios-1 during its 20 successive trajectories from 0.3 to 1 AU (January 1975-December 1979). This epoch analysis is similar to that of Zhang and Burlaga. Because data are not taken at a fixed (1 AU) but rather at different distances (Helios-1), all hourly values used are normalized to 1 AU (i.e., temperature, density and magnetic field). After the application of the above-mentioned criteria for closed structure development, applied for the whole 5-year period, about 50 hourly values fulfilling them have been found. The selected values are part of several closed structures the characteristic parameters of which are superposed. This analysis shows a unique behaviour of alpha particles inside magnetically closed structures, which however does not exclude their being influenced by such structures.     

Modification of the lunar surface by solar wind ion bombardment

Trivalent osmium ions are substitutionally incorporated into aqueous precipitates and melt-grown single crystals of AgBr and AgC1. The ions are distributed between three structurally inequivalent lattice sites in both salts. From epr studies, we have inferred that these sites are distinguished by the arrangement of charge-compensating silver ion vacancies in the two closest cation subshells. The most reasonable dopant-vacancy configurations have been deduced from the epr data. These configurations persist up to at least 300 K, and are compared with those observed in other trivalent metal ion doped systems.     

Gyrokinetic simulations of solar wind turbulence from ion to electron scales

A three-dimensional, nonlinear gyrokinetic simulation of plasma turbulence resolving scales from the ion to electron gyroradius with a realistic mass ratio is presented, where all damping is provided by resolved physical mechanisms. The resulting energy spectra are quantitatively consistent with a magnetic power spectrum scaling of k(-2.8) as observed in in situ spacecraft measurements of the "dissipation range" of solar wind turbulence. Despite the strongly nonlinear nature of the turbulence, the linear kinetic Alfvén wave mode quantitatively describes the polarization of the turbulent fluctuations. The collisional ion heating is measured at subion-Larmor radius scales, which provides evidence of the ion entropy cascade in an electromagnetic turbulence simulation.     

On the origin of solar wind. Alfvén waves induced jump of coronal temperature

Absorption of Alfvén waves is considered to be the main mechanism of heating in the solar corona. It is concluded that the sharp increase of the plasma temperature by two orders of magnitude is related to a self-induced opacity with respect to Alfvén waves. The maximal frequency for propagation of Alfvén waves is determined by the strongly temperature dependent kinematic viscosity. In such a way the temperature jump is due to absorption of high frequency Alfvén waves in a narrow layer above the solar surface. It is calculated the power per unit area dissipated in this layer due to damping of Alfvén waves that blows up the plasma and gives birth to the solar wind. A model short wave-length (WKB) evaluation takes into account the 1/f² frequency dependence of the transversal magnetic field and velocity spectral densities. Such spectral densities agree with old magnetometric data taken by Voyager 1 and recent theoretical calculations in the framework of Langevin-Burgers MHD. The presented theory predicts existence of intensive high frequency MHD Alfvén waves in the cold layer beneath the corona. It is briefly discussed how this statement can be checked experimentally. It is demonstrated that the magnitude of the Alfvén waves generating random noise and the solar wind velocity can be expressed only in terms of satellite experimental data. It is advocated that investigation of properties of the solar surface as a random driver by optical methods is an important task for future solar physics.     

Small-scale ion flux and magnetic field fluctuations in solar wind, foreshock and magnetosheath

We have continued investigation of waves in the regions of undisturbed solar wind, foreshock and magnetosheath. The analysis of ion flux and magnetic field variations with the time interval 1-240s was performed in the regions above. Very large variation in such a time interval can be considered the common feature of the foreshock and magnetosheath. The results of case and statistical studies showed that the level of relative variations of ion flux and magnetic field magnitude in foreshock is about 3 times larger than in undisturbed solar wind. Variations of these parameters in the magnetosheath topologically connected with the quasi-parallel bow shock are about two times larger than those behind the quasi-perpendicular. We also compared the results from Interball-1 data analysis with those from statistical analysis of cluster magnetic field measurements. The magnetic field variations obtained from the different satellite data coincide with each other very well not only in quality but also in quantity.     

Non-equilibrium ionization and electron density in the coronal plasma during solar flares

Summary The Li-like to He-like ion population ratio for calcium at the onset of solar flares is observed to be about 60% higher than in steady-state ionization balance. The measurement of the duration of this initial period of transient ionization and of the population ratios of adjacent ionization states allows an estimate of the electron density of the coronal plasma at flare onset. The density found in this study, within 1·10⁹ and 7·10⁹ cm⁻³ is comparable with the density typical of pre-flare active regions.     

Origin and evolution of MHD turbulence in the solar wind

Summary Solar wind turbulence has both solar and interplanetary sources. Outward travelling waves are generated at the Sun with a spectrum related to the turbulent processes in the solar atmosphere. Instabilities at velocity shears give a local contribution of waves with inward and outward propagation. Nonlinear interactions between the two kinds of waves lead to an energy cascade and to a Kolmogoroff spectrum. To speed up publication, the proofs were not sent to the authors and were supervised by the Scientific Committee.     

Compressibility in solar wind plasma turbulence

Incompressible magnetohydrodynamics is often assumed to describe solar wind turbulence. We use extended self-similarity to reveal scaling in the structure functions of density fluctuations in the solar wind. The obtained scaling is then compared with that found in the inertial range of quantities identified as passive scalars in other turbulent systems. We find that these are not coincident. This implies that either solar wind turbulence is compressible or that straightforward comparison of structure functions does not adequately capture its inertial range properties.     

Modified temperature-anisotropy instability thresholds in the solar wind

The proton and electron temperature anisotropies in the solar wind are constrained by the instability thresholds for temperature-anisotropy-driven kinetic plasma instabilities. The modifications to the marginal instability conditions from accounting for the influence of damping connected with the collisional effects in the solar wind plasma are calculated for right- and left-handed polarized parallel propagating Alfvén waves and mirror and firehose fluctuations. These modifications provide tighter threshold constraints compared to the marginal thresholds but do not fully explain the observations at small values of the parallel plasma beta.     

Magnetic discontinuities in magnetohydrodynamic turbulence and in the solar wind

Recent measurements of solar wind turbulence report the presence of intermittent, exponentially distributed angular discontinuities in the magnetic field. In this Letter, we study whether such discontinuities can be produced by magnetohydrodynamic (MHD) turbulence. We detect the discontinuities by measuring the fluctuations of the magnetic field direction, Δθ, across fixed spatial increments Δx in direct numerical simulations of MHD turbulence with an imposed uniform guide field B(0). A large region of the probability density function (pdf) for Δθ is found to follow an exponential decay, proportional to exp(-Δθ/θ(*)), with characteristic angle θ(*)≈(14°)(b(rms)/B(0))(0.65) for a broad range of guide-field strengths. We find that discontinuities observed in the solar wind can be reproduced by MHD turbulence with reasonable ratios of b(rms)/B(0). We also observe an excess of small angular discontinuities when Δx becomes small, possibly indicating an increasing statistical significance of dissipation-scale structures. The structure of the pdf in this case closely resembles the two-population pdf seen in the solar wind. We thus propose that strong discontinuities are associated with inertial-range MHD turbulence, while weak discontinuities emerge from dissipation-range turbulence. In addition, we find that the structure functions of the magnetic field direction exhibit anomalous scaling exponents, which indicates the existence of intermittent structures.     

Chaos in the solar wind flow near Earth

We have done a time series analysis of daily average data of solar wind velocity, density and temperature at 1 AU measured by ACE spacecraft for a period of nine years. We have used the raw data without filtering to give a faithful representation of the nonlinear behaviour of the solar wind flow which is a novel one. The sensitivity of the results on filtering is highlighted. The attractor dimension is estimated for every parameter of the solar wind and it is found that they differ substantially. Hence a chaotic picture for the problem from different angles have been obtained. The calculated Kolmogorov entropies and Lyapunov exponents are positive showing evidences that the complex solar wind near the Earth is most likely a deterministic chaotic system.      

Resistive instabilities of current sheets in the solar wind

Summary We present some numerical results on resistive magnetohydrodynamic instabilities and discuss their relevance to current sheets of the type indicated by spacecraft observations in the interplanetary plasma.

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Riassunto Si presentano dei risultati numerici sulle instabilità magnetoidrodinamiche resistive. Si discute inoltre la loro rilevanza per l'origine di strati di corrente che sono osservati da satelliti nel mezzo interplanetario.

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Резюме Мы приводим некоторые численные результаты по магнитноги-дродинамическим неустойчивостям, связанным с активным сопротивлением. Обсуждается их причастность к токовым слоям обнаруженным при наблюдениян на космическин аппаратах в межпланетной плазме.

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To speed up publication, the authors of this paper have agreed to not receive the proofs for correction.     

Observations of nonlinear turbulence in the upstream solar wind

Summary Plasma, electric-field and magnetic-field data from several experiments on board the spacecraft ISEE 1 and 2 have been analysed in the interaction region upstream of the Earth's bow shock. Upstream waves which are known to be associated with diffuse distributions of backstreaming protons are shown to correlate also with variability in the distribution of the incoming solar-wind protons. Both phenomena are also clearly connected with the presence of enhanced electric-field turbulence. On the basis of these relations, a preliminary discussion can be given of the complex nonlinear plasma processes occurring in the foreshock region.