Observation of the Hot Electron Interchange Instability in a High Beta Dipolar Confined Plasma
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Analysis of Plasma Instabilities and Verification of the BOUT Code for The
Analysis of plasma instabilities and verification of the BOUT code for the Large Plasma Device P. Popovich,1 M.V. Umansky,2 T.A. Carter,1, a) and B. Friedman1 1)Department of Physics and Astronomy and Center for Multiscale Plasma Dynamics, University of California, Los Angeles, CA 90095-1547 2)Lawrence Livermore National Laboratory, Livermore, CA 94550, USA (Dated: 8 August 2018) The properties of linear instabilities in the Large Plasma Device [W. Gekelman et al., Rev. Sci. Inst., 62, 2875 (1991)] are studied both through analytic calculations and solving numerically a system of linearized collisional plasma fluid equations using the 3D fluid code BOUT [M. Umansky et al., Contrib. Plasma Phys. 180, 887 (2009)], which has been successfully modified to treat cylindrical geometry. Instability drive from plasma pressure gradients and flows is considered, focusing on resistive drift waves, the Kelvin-Helmholtz and rotational interchange instabilities. A general linear dispersion relation for partially ionized collisional plasmas including these modes is derived and analyzed. For LAPD relevant profiles including strongly driven flows it is found that all three modes can have comparable growth rates and frequencies. Detailed comparison with solutions of the analytic dispersion relation demonstrates that BOUT accurately reproduces all characteristics of linear modes in this system. PACS numbers: 52.30.Ex, 52.35.Fp, 52.35.Kt, 52.35.Lv, 52.65.Kj arXiv:1004.4674v4 [physics.plasm-ph] 26 Jan 2011 a)Electronic mail: [email protected] 1 I. INTRODUCTION Understanding complex nonlinear phenomena in magnetized plasmas increasingly relies on the use of numerical simulation as an enabling tool. -
Shear Flow-Interchange Instability in Nightside Magnetotail Causes Auroral Beads As a Signature of Substorm Onset
manuscript submitted to JGR: Space Physics Shear flow-interchange instability in nightside magnetotail causes auroral beads as a signature of substorm onset Jason Derr1, Wendell Horton1, Richard Wolf2 1Institute for Fusion Studies and Applied Research Laboratories, University of Texas at Austin 2Physics and Astronomy Department, Rice University Key Points: • A wedge model is extended to obtain a MHD magnetospheric wave equation for the near-Earth magnetotail, including velocity shear effects. • Shear flow-interchange instability to replace shear flow-ballooning and interchange in- stabilities as substorm onset cause. • WKB applicability conditions suggest nonlinear analysis is necessary and yields spatial scale of most unstable mode’s variations. arXiv:1904.11056v1 [physics.space-ph] 24 Apr 2019 Corresponding author: Jason Derr, [email protected] –1– manuscript submitted to JGR: Space Physics Abstract A geometric wedge model of the near-earth nightside plasma sheet is used to derive a wave equation for low frequency shear flow-interchange waves which transmit E~ × B~ sheared zonal flows along magnetic flux tubes towards the ionosphere. Discrepancies with the wave equation result used in Kalmoni et al. (2015) for shear flow-ballooning instability are dis- cussed. The shear flow-interchange instability appears to be responsible for substorm onset. The wedge wave equation is used to compute rough expressions for dispersion relations and local growth rates in the midnight region of the nightside magnetotail where the instability develops, forming the auroral beads characteristic of geomagnetic substorm onset. Stability analysis for the shear flow-interchange modes demonstrates that nonlinear analysis is neces- sary for quantitatively accurate results and determines the spatial scale on which the instability varies. -
Stability Study of the Cylindrical Tokamak--Thomas Scaffidi(2011)
Ecole´ normale sup erieure´ Princeton Plasma Physics Laboratory Stage long de recherche, FIP M1 Second semestre 2010-2011 Stability study of the cylindrical tokamak Etude´ de stabilit´edu tokamak cylindrique Author: Supervisor: Thomas Scaffidi Prof. Stephen C. Jardin Abstract Une des instabilit´es les plus probl´ematiques dans les plasmas de tokamak est appel´ee tearing mode . Elle est g´en´er´ee par les gradients de courant et de pression et implique une reconfiguration du champ magn´etique et du champ de vitesse localis´ee dans une fine r´egion autour d’une surface magn´etique r´esonante. Alors que les lignes de champ magn´etique sont `al’´equilibre situ´ees sur des surfaces toriques concentriques, l’instabilit´econduit `ala formation d’ˆıles magn´etiques dans lesquelles les lignes de champ passent d’un tube de flux `al’autre, rendant possible un trans- port thermique radial important et donc cr´eant une perte de confinement. Pour qu’il puisse y avoir une reconfiguration du champ magn´etique, il faut inclure la r´esistivit´edu plasma dans le mod`ele, et nous r´esolvons donc les ´equations de la magn´etohydrodynamique (MHD) r´esistive. On s’int´eresse `ala stabilit´ede configurations d’´equilibre vis-`a-vis de ces instabilit´es dans un syst`eme `ala g´eom´etrie simplifi´ee appel´ele tokamak cylindrique. L’´etude est `ala fois analytique et num´erique. La solution analytique est r´ealis´ee par une m´ethode de type “couche limite” qui tire profit de l’´etroitesse de la zone o`ula reconfiguration a lieu. -
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Laboratory Investigation of the Dynamics of Shear Flows in a Plasma Boundary Layer by Ami Marie DuBois A dissertation submitted to the Graduate Faculty of Auburn University in partial fulfillment of the requirements for the Degree of Doctor of Philosophy Auburn, Alabama December 14, 2013 Copyright 2013 by Ami Marie DuBois Approved by Edward Thomas, Jr., Chair, Professor of Physics William Amatucci, Staff Scientist at Naval Research Laboratory Uwe Konopka, Professor of Physics David Maurer, Professor of Physics Abstract The laboratory experiments presented in this dissertation investigate a regime of instabilities that occur when a highly localized, radial electric field oriented perpendicular to a uniform background magnetic field gives rise to an azimuthal velocity shear profile at the boundary between two interpenetrating plasmas. This investigation is motivated by theoretical predictions which state that plasmas are unstable to transverse and parallel inhomogeneous sheared flows over a very broad frequency range. Shear driven instabilities are commonly observed in the near-Earth space environment when boundary layers, such as the magnetopause and the plasma sheet boundary layer, are compressed by intense solar storms. When the shear scale length is much less than the ion gyro- radius, but greater than the electron gyro-radius, the electrons are magnetized in the shear layer, but the ions are effectively un-magnetized. The resulting shear driven instability, the electron-ion hybrid instability, is investigated in a new interpenetrating plasma configuration in the Auburn Linear EXperiment for Instability Studied (ALEXIS) in the absence of a magnetic field aligned current. In order to truly understand the dynamics at magnetospheric boundary layers, the EIH instability is studied in the presence of a density gradient located at the boundary layer between two plasmas. -
Interchange Instability and Transport in Matter-Antimatter Plasmas
WPEDU-PR(18) 20325 A Kendl et al. Interchange Instability and Transport in Matter-Antimatter Plasmas. Preprint of Paper to be submitted for publication in Physical Review Letters This work has been carried out within the framework of the EUROfusion Con- sortium and has received funding from the Euratom research and training pro- gramme 2014-2018 under grant agreement No 633053. The views and opinions expressed herein do not necessarily reflect those of the European Commission. This document is intended for publication in the open literature. It is made available on the clear under- standing that it may not be further circulated and extracts or references may not be published prior to publication of the original when applicable, or without the consent of the Publications Officer, EUROfu- sion Programme Management Unit, Culham Science Centre, Abingdon, Oxon, OX14 3DB, UK or e-mail Publications.Offi[email protected] Enquiries about Copyright and reproduction should be addressed to the Publications Officer, EUROfu- sion Programme Management Unit, Culham Science Centre, Abingdon, Oxon, OX14 3DB, UK or e-mail Publications.Offi[email protected] The contents of this preprint and all other EUROfusion Preprints, Reports and Conference Papers are available to view online free at http://www.euro-fusionscipub.org. This site has full search facilities and e-mail alert options. In the JET specific papers the diagrams contained within the PDFs on this site are hyperlinked Interchange instability and transport in matter-antimatter plasmas Alexander Kendl, Gregor Danler, Matthias Wiesenberger, Markus Held Institut f¨ur Ionenphysik und Angewandte Physik, Universit¨at Innsbruck, Technikerstr. -
View Technical Report
CH9700652 LRP 581/97 August 1997 Global approach to the spectral problem of MICROINSTABILITIES IN TOKAMAK PLASMAS USING A GYROKINETIC MODEL S. Brunner CRPP Centre de Recherches en Physique des Plasmas ECOLE POLYTECHNIQUE Association Euratom - Confederation Suisse FEDERALE DE LAUSANNE Centre de Recherches en Physique des Plasmas (CRPP) Association Euratom - Confederation Suisse Ecole Poly technique Federate de Lausanne PPB, CH-1015 Lausanne, Switzerland phone: +41 21 693 34 82 17 —fax +41 21 693 51 76 Centre de Recherches en Physique des Plasmas - Technologle de la Fusion (CRPP-TF) Association Euratom - Confederation Suisse Ecole Poly technique Federate de Lausanne CH-5232 Vllligen-PSI, Switzerland phone: +41 56 310 32 59 —fax +41 56 310 37 29 LRP 581/97 August 1997 Global approach to the spectral problem of MICROINSTABILITIES IN TOKAMAK PLASMAS USING A GYROKINET1C MODEL S. Brunner EPFL 1997 Abstract Ion temperature gradient (ITG) -related instabilities are studied in tokamak-like plas mas with the help of a new global eigenvalue code. Ions are modeled in the frame of gyrokinetic theory so that finite Larmor radius effects of these particles are retained to all orders. Non-adiabatic trapped electron dynamics is taken into account through the bounce-averaged drift kinetic equation. Assuming electrostatic perturbations, the sys tem is closed with the quasineutrality relation. Practical methods are presented which make this global approach feasible. These include a non-standard wave decomposition compatible with the curved geometry as well as adapting an efficient root finding al gorithm for computing the unstable spectrum. These techniques are applied to a low pressure configuration given by a large aspect ratio torus with circular, concentric mag netic surfaces. -
Dynamics of the J Avian Magnetosphere
25 Dynamics of the J avian Magnetosphere N. Krupp, V. M. Vasyliunas, J. Woch, A. Lagg Max-Planck-Institut fur Sonnensystemforschung, Katlenburg-Lindau K. K. Khurana, M. G. Kivelson IGPP and Dept. Earth & Space Sciences, University of California, Los Angeles B. H. Mauk, E. C. Roelof, D. J. Williams, S. M. Krimigis The Johns Hopkins University Applied Physics Laboratory W. S. Kurth, L. A. Frank, W. R. Paterson Dept. of Physics & As.tronomy, University of Iowa 25.1 INTRODUCTION around Jupiter for almost 8 years (1995-2003), Galileo has collected in situ data of the jovian system over an extended Understanding the dynamic processes in the largest magne duration and has for the first time made possible the study tosphere of our solar system is one of the outstanding goals of Jupiter on timescales of weeks, months, and even years, of magnetospheric physics. These processes are associated using the same instrumentation. New regions of the jovian with temporal and/ or spatial variations of the global config magnetosphere have been explored, especially the jovian uration. Their timescales range from several tens of minutes magnetotail which was not visited by any of the previous to sizeable fractions of the planetary rotation period to long spacecraft (except, to a very minor extent, by Voyager 2). term variations which take several days to develop. They oc Additional inputs have become available from ground-based cur on both local and global spatial scales, out to dimensions and Earth-orbit-based measurements and from advanced representing a large fraction of the magnetosphere. global magneto hydrodynamic (MHD) simulations of the jo Early indications of a "living", varying jovian magneto vian magnetosphere. -
Dynamics of the Saturnian Inner Magnetosphere: First Inferences from the Cassini Magnetometers About Small-Scale Plasma Transport in the Magnetosphere N
GEOPHYSICAL RESEARCH LETTERS, VOL. 32, L14S06, doi:10.1029/2005GL022643, 2005 Dynamics of the Saturnian inner magnetosphere: First inferences from the Cassini magnetometers about small-scale plasma transport in the magnetosphere N. Andre´ Centre d’Etudes Spatiales des Rayonnements, Toulouse, France M. K. Dougherty Blackett Laboratory, Space and Atmospheric Physics, Imperial College, London, UK C. T. Russell, J. S. Leisner, and K. K. Khurana Institute of Geophysics and Planetary Physics, University of California, Los Angeles, USA Received 7 February 2005; revised 18 April 2005; accepted 16 May 2005; published 14 June 2005. [1] The Cassini magnetometers reveal a very dynamic and neutral sources [Richardson, 1998] and include the plasmadisc within the inner Saturnian magnetosphere planetary ionosphere, the main ring system, the more during the first three orbits of the Cassini orbital tour. diffuse E-ring, and numerous icy satellites (Mimas, This corotation-dominated region is known to contain Enceladus, Tethys, Dione, and Rhea). Titan which is various neutral and plasma populations and Voyager the other dominant plasma source at Saturn resides in spacecraft observations suggest important radial transport the outer magnetospheric regions at a radial distance of processes redistribute the locally created plasma out to the 20 Rs. remote magnetospheric regions, by a mechanism yet to be [4] The plasma created by the internal distributed sources identified. In this work we report on anomalous magnetic is trapped by the planetary magnetic field and confined to field signatures in the inner regions of the magnetosphere the equatorial plane by the centrifugal force, thereby giving (inside of 8 Saturn radii) that may participate in the radial rise to a thin disc of corotating plasma in the inner transport and that seem to be consistent with signatures of magnetospheric regions. -
Are Saturn's Interchange Injections Organized by Rotational Longitude?
Azari Abigail, R. (Orcid ID: 0000-0002-8665-5459) Jia Xianzhe (Orcid ID: 0000-0002-8685-1484) Liemohn Michael, W. (Orcid ID: 0000-0002-7039-2631) Hospodarsky George, Blair (Orcid ID: 0000-0001-9200-9878) Provan Gabrielle (Orcid ID: 0000-0001-7442-4154) Ye Sheng-Yi (Orcid ID: 0000-0002-3064-1082) Cowley Stanley, W. H. (Orcid ID: 0000-0002-4041-0034) Paranicas Christopher, P. (Orcid ID: 0000-0002-4391-8255) Sergis Nick (Orcid ID: 0000-0003-4144-8699) Rymer Abigail, Mary (Orcid ID: 0000-0002-4879-0748) Thomsen Michelle, F. (Orcid ID: 0000-0003-0140-9265) Mitchell Donald, G. (Orcid ID: 0000-0003-1960-2119) Are Saturn’s Interchange Injections Organized by Rotational Longitude? A. R. Azari1, X. Jia1, M. W. Liemohn1, G. B. Hospodarsky2, G. Provan3, S. -Y. Ye2, S. W. H. Cowley3, C. Paranicas4, N. Sergis5, 6, A. M. Rymer4, M. F. Thomsen7, and D. G. Mitchell4 1Department of Climate and Space Sciences and Engineering, University of Michigan, Ann Arbor, Michigan, USA. 2Department of Physics and Astronomy, University of Iowa. 3Department of Physics and Astronomy, University of Leicester, Leicester, UK. 4The Johns Hopkins University Applied Physics Laboratory, 5Office of Space Research and Technology, Academy of Athens, 6Institute for Astronomy, Astrophysics, Space Applications and Remote Sensing, National Observatory of Athens, 7Planetary Science Institute. Corresponding author: A. R. Azari ([email protected]) Key Points: • Interchange injections, identified from an automated detection method, shows strongest organization in local time compared to longitude • Longitude system dependence of equatorial interchange injections exists but it is weak and inconsistent to previous works • Interchange occurrence rates weakly peak at ~90° in northern SLS-5 and PPO between 7 – 9 Saturn Radii but occur at all longitudes and seasons This is the author manuscript accepted for publication and has undergone full peer review but has not been through the copyediting, typesetting, pagination and proofreading process, which may lead to differences between this version and the Version of Record. -
Partially Ionized Plasmas in Astrophysics
Space Sci Rev (2018) 214:58 https://doi.org/10.1007/s11214-018-0485-6 Partially Ionized Plasmas in Astrophysics José Luis Ballester1 · Igor Alexeev2 · Manuel Collados3 · Turlough Downes4 · Robert F. Pfaff5 · Holly Gilbert6 · Maxim Khodachenko7 · Elena Khomenko3 · Ildar F. Shaikhislamov8 · Roberto Soler1 · Enrique Vázquez-Semadeni9 · Teimuraz Zaqarashvili7,10 Received: 29 June 2017 / Accepted: 2 February 2018 © Springer Science+Business Media B.V., part of Springer Nature 2018 Abstract Partially ionized plasmas are found across the Universe in many different as- trophysical environments. They constitute an essential ingredient of the solar atmosphere, molecular clouds, planetary ionospheres and protoplanetary disks, among other environ- ments, and display a richness of physical effects which are not present in fully ionized plasmas. This review provides an overview of the physics of partially ionized plasmas, in- cluding recent advances in different astrophysical areas in which partial ionization plays a B J.L. Ballester [email protected] I. Alexeev [email protected] M. Collados [email protected] T. Downes [email protected] R.F. Pfaff [email protected] H. Gilbert [email protected] M. Khodachenko [email protected] E. Khomenko [email protected] I.F. Shaikhislamov [email protected] R. Soler [email protected] E. Vázquez-Semadeni [email protected] T. Zaqarashvili [email protected] 58 Page 2 of 149 J.L. Ballester et al. fundamental role. We outline outstanding observational and theoretical questions and dis- cuss possible directions for future progress. Keywords Plasmas · Magnetohydrodynamics · Sun · Molecular clouds · Ionospheres · Exoplanets 1 Introduction Plasma pervades the Universe at all scales, and the term plasma universe was coined by Hannes Alfvén to point out the important role played by plasmas across the universe (Alfven 1986). -
Rayleigh-Taylor Interchange Instability in a Magnetized Fluid And, in The
PFC/JA-87-10 MHD CLUMP INSTABILITY by D.J. Tetreault Massachusetts Institute of Technology Cambridge, MA 02139 January 1987 Submitted to The Physics of Fluids ABSTRACT The theory of MHD clump instability in a plasma with magnetic shear is presented. MHD clump fluctuations are produced when the mean magnetic field shear is turbulently mixed. Nonlinear instability results when, as the clump magnetic island structures resonantly overlap, the mixing overcomes clump decay due to magnetic field line stochasticity. The instability growth time is on the order of the Lyapunov time. The renormalized dynamical equation describing the MHD clump instability is derived from one fluid MHD equitions and conserves the dynamical invariants of the exact equations. The renormalized equation is a nonlinear, turbulent version of the Newcomb equation of linear MHD stability theory and can be cast into the form of a nonlinear MHD energy principle. The growth rate of the instability is calculated. The instability is a nonlinear analogue of the Rayleigh-Taylor interchange instability in a magnetized fluid and, in the 1 fully stochastic case, of the tearing mode instability. MHD clump instability is a dynamical route to the Taylor state. 2 I. INTRODUCTION It has been suggested that nonlinear fluctuations called clumps will occur in magnetohydrodynamic (MHD) plasma with magnetic shear.' Clumps were first discussed in studies of Vlasov turbulence, where the term was used to describe resonant fluctuations produced by the turbulent mixing of phase space density gradients . The clump fluctuations arise because the phase space density is conserved in a Vlasov plasma: an element of phase space density is turbulently transported to a new region of phase space of different density. -
Guiding Center Motion
GUIDING CENTER MOTION H.J. de Blank FOM Institute DIFFER – Dutch Institute for Fundamental Energy Research, Association EURATOM-FOM, P.O. Box 1207, 3430 BE Nieuwegein, The Netherlands, www.differ.nl. ABSTRACT Secondly, the Coulomb force is a long range interaction. In a well-ionized plasma, particles rarely suffer large-angle The motion of charged particles in slowly varying electro- deflections in two-particle collisions. Rather, their orbits are magnetic fields is analyzed. The strength of the magnetic deflected through weak interactions with many particles si- field is such that the gyro-period and the gyro-radius of the multaneously. Hence, the effects of collisions can be best particle motion around field lines are the shortest time and described statistically, in terms of distributions of particles. length scales of the system. The particle motion is described The kinetic equation for the particle distribution function as the sum of a fast gyro-motion and a slow drift velocity. will be discussed at the end of this chapter, with emphasis on the role of the particle orbits, not the collisions. The equations of motion of a particle with mass m and I. INTRODUCTION charge q in electromagnetic fields E(x, t) and B(x, t) are, The interparticle forces in ordinary gases are short-ranged, q x˙ = v, v˙ = (E + v B), (1) so that the constituent particles follow straight lines between m × collisions. At low densities where collisions become rare, N the gas molecules bounce up and down between the walls of where the dot denotes the time derivative. Each of the the containing vessel before experiencing a collision.