Significant advances have been made recently in both the theoretical understanding and observation of small-scale turbulence in different layers of the Sun, and in the instabilities that give rise to them. The general development of solar physics, however, has led to such a degree of specialization as to hinder interaction between workers in the field. This book therefore presents studies of different layers and regions of the Sun, but from the same aspect, concentrating on the study of small-scale motions. The main emphasis is on the common theoretical roots of these phenomena, but the book also contains an extensive treatment of the observational aspects.
|Other titles||Proceedings of the NATO Advanced Research Workshop, held in Lillafured, Hungary, 16-20 September 2002|
|Statement||edited by R. Erdélyi, K. Petrovay, B. Roberts, M. Aschwanden|
|Series||NATO Science Series II: Mathematics, Physics and Chemistry, 1568-2609 -- 124, NATO science series -- 124.|
|Contributions||Petrovay, K., Roberts, B., Aschwanden, M.|
|The Physical Object|
|Format||[electronic resource] :|
|Pagination||1 online resource (404 pages).|
|Number of Pages||404|
Get this from a library! Turbulence, waves, and instabilities in the solar plasma. [R Erdélyi;]. Turbulence, Waves and Instabilities in the Solar Plasma de - English books - commander la livre de la catégorie sans frais de port et bon marché - Ex Libris boutique en ligne. Turbulence, Waves and Instabilities in the Solar Plasma: Proceedings of the NATO Advanced Research Workshop on Turbulence, Waves, and Instabilities in September (Nato Science Series II:) (rd Edition). A chapter focuses on plasma turbulence, which results from the development of cyclotron instabilities. The last chapter discusses pertinent experimental data concerning cyclotron waves in plasma. The book is intended for specialists in plasma physics and a number of related fields, including the physics of the ionosphere, solar wind and.
Key words: instabilities – solar wind – turbulence – waves Supporting material: animation 1. INTRODUCTION Turbulence in magnetized weakly collisional space and astrophysical plasmas is a ubiquitous nonlinear phenomenon that allows energy transfer from large to small scales and, eventually, to plasma particles. Properties of plasma turbulence. The following topics will be addressed: Linear theory of magneto-Rossby waves, three-wave interactions and related parametric instabilities, zonal flows, and turbulence. Full article (This article belongs to the Special Issue Turbulence, Waves and Transport in Stratified, Rotating Fluid and Plasma Flows). This kind of phenomenon is found in various natural contexts and in different regimes, for instance, in the Earth's magnetosphere, where the establishment of a turbulent state follows Kelvin–Helmholtz or tearing instabilities; in the solar wind plasma, where turbulent fluctuations at ion scales can generate plasma micro-instabilities and out. Turbulence, Waves and Instabilities in the Solar Plasma: Proceedings of the NATO Advanced Research Workshop on Turbulence, Waves, and Instabilities in the Solar Plasma .
5 Page 6 of D. Verscharen et al. of its trajectory due to the Lorentz force. The frequency associated with this helical motion is given by the gyro-frequency1 (also called the cyclotron frequency) Ωj ≡ qj B0 mjc, (3) where c is the speed of light in vacuum. The timescale for one closed loop around the. In this presentation we will focus on some of the early science return made possible by the Solar Probe Plus mission, and more specifically the returns from the first three perihelia at solar radii (Rs), just over half the distance from the Sun of the previous closest approaching spacecraft, Helios ( Rs). The increased exploration of the inner heliosphere will allow important new. We show that aperiodic mirror instabilities of slow MHD waves can develop under solar coronal conditions for weak magnetic fields (B instabilities can develop for. The parametric instabilities of an Alfvén wave in a proton-electron plasma system are found to have great influence on proton dynamics, where part of the protons can be accelerated through the Landau resonance with the excited ion acoustic waves, and a beam component along the .