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Small-Scale Dynamo Action in Rotating Compressible Convection
Small-scale dynamo action in rotating compressible convection B. Favier∗and P.J. Bushby School of Mathematics and Statistics, Newcastle University, Newcastle upon Tyne NE1 7RU, UK Abstract We study dynamo action in a convective layer of electrically-conducting, compressible fluid, rotating about the vertical axis. At the upper and lower bounding surfaces, perfectly- conducting boundary conditions are adopted for the magnetic field. Two different levels of thermal stratification are considered. If the magnetic diffusivity is sufficiently small, the con- vection acts as a small-scale dynamo. Using a definition for the magnetic Reynolds number RM that is based upon the horizontal integral scale and the horizontally-averaged velocity at the mid-layer of the domain, we find that rotation tends to reduce the critical value of RM above which dynamo action is observed. Increasing the level of thermal stratification within the layer does not significantly alter the critical value of RM in the rotating calculations, but it does lead to a reduction in this critical value in the non-rotating cases. At the highest computationally-accessible values of the magnetic Reynolds number, the saturation levels of the dynamo are similar in all cases, with the mean magnetic energy density somewhere be- tween 4 and 9% of the mean kinetic energy density. To gain further insights into the differences between rotating and non-rotating convection, we quantify the stretching properties of each flow by measuring Lyapunov exponents. Away from the boundaries, the rate of stretching due to the flow is much less dependent upon depth in the rotating cases than it is in the corre- sponding non-rotating calculations. -
Effects of a Uniform Magnetic Field on a Growing Or Collapsing Bubble in a Weakly Viscous Conducting Fluid K
Effects of a uniform magnetic field on a growing or collapsing bubble in a weakly viscous conducting fluid K. H. Kang, I. S. Kang, and C. M. Lee Citation: Phys. Fluids 14, 29 (2002); doi: 10.1063/1.1425410 View online: http://dx.doi.org/10.1063/1.1425410 View Table of Contents: http://pof.aip.org/resource/1/PHFLE6/v14/i1 Published by the American Institute of Physics. Related Articles Dynamics of magnetic chains in a shear flow under the influence of a uniform magnetic field Phys. Fluids 24, 042001 (2012) Travelling waves in a cylindrical magnetohydrodynamically forced flow Phys. Fluids 24, 044101 (2012) Two-dimensional numerical analysis of electroconvection in a dielectric liquid subjected to strong unipolar injection Phys. Fluids 24, 037102 (2012) Properties of bubbled gases transportation in a bromothymol blue aqueous solution under gradient magnetic fields J. Appl. Phys. 111, 07B326 (2012) Magnetohydrodynamic flow of a binary electrolyte in a concentric annulus Phys. Fluids 24, 037101 (2012) Additional information on Phys. Fluids Journal Homepage: http://pof.aip.org/ Journal Information: http://pof.aip.org/about/about_the_journal Top downloads: http://pof.aip.org/features/most_downloaded Information for Authors: http://pof.aip.org/authors Downloaded 07 May 2012 to 132.236.27.111. Redistribution subject to AIP license or copyright; see http://pof.aip.org/about/rights_and_permissions PHYSICS OF FLUIDS VOLUME 14, NUMBER 1 JANUARY 2002 Effects of a uniform magnetic field on a growing or collapsing bubble in a weakly viscous conducting fluid K. H. Kang Department of Mechanical Engineering, Pohang University of Science and Technology, San 31, Hyoja-dong, Pohang 790-784, Korea I. -
Magnetohydrodynamics
Magnetohydrodynamics J.W.Haverkort April 2009 Abstract This summary of the basics of magnetohydrodynamics (MHD) as- sumes the reader is acquainted with both fluid mechanics and electro- dynamics. The content is largely based on \An introduction to Magneto- hydrodynamics" by P.A. Davidson. The basic equations of electrodynam- ics are summarized, the assumptions underlying MHD are exposed and a selection of aspects of the theory are discussed. Contents 1 Electrodynamics 2 1.1 The governing equations . 2 1.2 Faraday's law . 2 2 Magnetohydrodynamical Equations 3 2.1 The assumptions . 3 2.2 The equations . 4 2.3 Some more equations . 4 3 Concepts of Magnetohydrodynamics 5 3.1 Analogies between fluid mechanics and MHD . 5 3.2 Dimensionless numbers . 6 3.3 Lorentz force . 7 1 1 Electrodynamics 1.1 The governing equations The Maxwell equations for the electric and magnetic fields E and B in vacuum are written in terms of the sources ρe (electric charge density) and J (electric current density) ρ r · E = e Gauss's law (1) "0 @B r × E = − Faraday's law (2) @t r · B = 0 No monopoles (3) @E r × B = µ J + µ " Ampere's law (4) 0 0 0 @t with "0 the electric permittivity and µ0 the magnetic permeability of free space. The electric field can be thought to consist of a static curl-free part Es = @A −∇V and an induced or in-stationary part Ei = − @t which is divergence-free, with V the electric potential and A the magnetic vector potential. The force on a charge q moving with velocity u is given by the Lorentz force f = q(E+u×B). -
Astrophysical Fluid Dynamics: II. Magnetohydrodynamics
Winter School on Computational Astrophysics, Shanghai, 2018/01/30 Astrophysical Fluid Dynamics: II. Magnetohydrodynamics Xuening Bai (白雪宁) Institute for Advanced Study (IASTU) & Tsinghua Center for Astrophysics (THCA) source: J. Stone Outline n Astrophysical fluids as plasmas n The MHD formulation n Conservation laws and physical interpretation n Generalized Ohm’s law, and limitations of MHD n MHD waves n MHD shocks and discontinuities n MHD instabilities (examples) 2 Outline n Astrophysical fluids as plasmas n The MHD formulation n Conservation laws and physical interpretation n Generalized Ohm’s law, and limitations of MHD n MHD waves n MHD shocks and discontinuities n MHD instabilities (examples) 3 What is a plasma? Plasma is a state of matter comprising of fully/partially ionized gas. Lightening The restless Sun Crab nebula A plasma is generally quasi-neutral and exhibits collective behavior. Net charge density averages particles interact with each other to zero on relevant scales at long-range through electro- (i.e., Debye length). magnetic fields (plasma waves). 4 Why plasma astrophysics? n More than 99.9% of observable matter in the universe is plasma. n Magnetic fields play vital roles in many astrophysical processes. n Plasma astrophysics allows the study of plasma phenomena at extreme regions of parameter space that are in general inaccessible in the laboratory. 5 Heliophysics and space weather l Solar physics (including flares, coronal mass ejection) l Interaction between the solar wind and Earth’s magnetosphere l Heliospheric -
Toward a Self-Generating Magnetic Dynamo: the Role of Turbulence
PHYSICAL REVIEW E VOLUME 61, NUMBER 5 MAY 2000 Toward a self-generating magnetic dynamo: The role of turbulence Nicholas L. Peffley, A. B. Cawthorne, and Daniel P. Lathrop* Department of Physics, University of Maryland, College Park, Maryland 20742 ͑Received 6 July 1999͒ Turbulent flow of liquid sodium is driven toward the transition to self-generating magnetic fields. The approach toward the transition is monitored with decay measurements of pulsed magnetic fields. These mea- surements show significant fluctuations due to the underlying turbulent fluid flow field. This paper presents experimental characterizations of the fluctuations in the decay rates and induced magnetic fields. These fluc- tuations imply that the transition to self-generation, which should occur at larger magnetic Reynolds number, will exhibit intermittent bursts of magnetic fields. PACS number͑s͒: 47.27.Ϫi, 47.65.ϩa, 05.45.Ϫa, 91.25.Cw I. INTRODUCTION Reynolds number will be quite large for all flows attempting to self-generate ͑where Re ӷ1 yields Reӷ105)—implying The generation of magnetic fields from flowing liquid m turbulent flow. These turbulent flows will cause the transition metals is being pursued by a number of scientific research to self-generation to be intermittent, showing both growth groups in Europe and North America. Nuclear engineering and decay of magnetic fields irregularly in space and time. has facilitated the safe use of liquid sodium, which has con- This intermittency is not something addressed by kinematic tributed to this new generation of experiments. With the dynamo studies. The analysis in this paper focuses on three highest electrical conductivity of any liquid, sodium retains main points: we quantify the approach to self-generation and distorts magnetic fields maximally before they diffuse with increasing Rem , characterize the turbulence of induced away. -
Magnetohydrodynamics
MAGNETOHYDRODYNAMICS International Max-Planck Research School. Lindau, 9{13 October 2006 {4{ Bulletin of exercises n◦4: The magnetic induction equation. 1. The induction equation: Starting from Faraday's law and Ampere's law (neglecting the displacement current) and making use of Ohm's constitutive relation, eliminate the electric field and the current density to obtain the inducion equation for a plasma in the MHD approximation: @B c2 = rot (v B) rot rot B : (1) @t ^ − 4πσe ! Show that if the electrical conductivity is uniform, the induction equation can be cast into the form @B = rot (v B) + η 2 B ; (2) @t ^ r def 2 where η = c =(4πσe) is the \magnetic diffusivity." 2. Combined form of the induction and the continuity equations. Show that the induction equation can be combined with the equation of continuity into one single differential equation which gives the time evolution of B/ρ following a fluid element, viz: D B B 1 = v rot (η rot B) : (3) D t ρ ! ρ · r! − ρ In the case of an ideal MHD-plasma, Eq. (3) simplifies to a form known as Wal´en's equation. 3. Strength of a magnetic flux tube. A magnetic flux tube is the region enclosed by the surface determined by all magnetic field lines passing through a given material circuit Ct . The \strength" of a flux tube is defined as the circulation of the potential vector A along the material circuit Ct , viz. ξ def def 2 Φm(t) = A d α = A[α(ξ; t)] α0(ξ; t) d ξ ; (4) ICt · Zξ1 · where α = α(ξ; t) is the parametric expression of the circuit Ct . -
Turbulent Dynamos: Experiments, Nonlinear Saturation of the Magnetic field and field Reversals
Turbulent dynamos: Experiments, nonlinear saturation of the magnetic field and field reversals C. Gissinger & C. Guervilly November 17, 2008 1 Introduction Magnetic fields are present at almost all scales in the universe, from the Earth (roughly 0:5 G) to the Galaxy (10−6 G). It is commonly believed that these magnetic fields are generated by dynamo action i.e. by the turbulent flow of an electrically conducting fluid [12]. Despite this space and time disorganized flow, the magnetic field shows in general a coherent part at the largest scales. The question arising from this observation is the role of the mean flow: Cowling first proposed that the coherent magnetic field could be due to coherent large scale velocity field and this problem is still an open question. 2 MHD equations and dimensionless parameters The equations describing the evolution of a magnetohydrodynamical system are the equation of Navier-Stokes coupled to the induction equation: @v 1 + (v )v = π + ν∆v + f + (B )B ; (1) @t · r −∇ µρ · r @B = (v B) + η ∆B : (2) @t r × × where v is the solenoidal velocity field, B the solenoidal magnetic field, π the pressure r gradient in the fluid, ν the kinematic viscosity, f a forcing term, µ the magnetic permeabil- ity, ρ the fluid density and η the magnetic permeability. Dealing with the geodynamo, the minimal set of parameters for the outer core are : ρ : density of the fluid • µ : magnetic permeability • 54 ν : kinematic diffusivity • σ: conductivity • R : radius of the outer core • V : typical velocity • Ω : rotation rate • The problem involves 7 independent parameters and 4 fundamental units (length L, time T , mass M and electic current A). -
Stability and Instability of Hydromagnetic Taylor-Couette Flows
Physics reports Physics reports (2018) 1–110 DRAFT Stability and instability of hydromagnetic Taylor-Couette flows Gunther¨ Rudiger¨ a;∗, Marcus Gellerta, Rainer Hollerbachb, Manfred Schultza, Frank Stefanic aLeibniz-Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany bDepartment of Applied Mathematics, University of Leeds, Leeds, LS2 9JT, United Kingdom cHelmholtz-Zentrum Dresden-Rossendorf, Bautzner Landstr. 400, D-01328 Dresden, Germany Abstract Decades ago S. Lundquist, S. Chandrasekhar, P. H. Roberts and R. J. Tayler first posed questions about the stability of Taylor- Couette flows of conducting material under the influence of large-scale magnetic fields. These and many new questions can now be answered numerically where the nonlinear simulations even provide the instability-induced values of several transport coefficients. The cylindrical containers are axially unbounded and penetrated by magnetic background fields with axial and/or azimuthal components. The influence of the magnetic Prandtl number Pm on the onset of the instabilities is shown to be substantial. The potential flow subject to axial fieldspbecomes unstable against axisymmetric perturbations for a certain supercritical value of the averaged Reynolds number Rm = Re · Rm (with Re the Reynolds number of rotation, Rm its magnetic Reynolds number). Rotation profiles as flat as the quasi-Keplerian rotation law scale similarly but only for Pm 1 while for Pm 1 the instability instead sets in for supercritical Rm at an optimal value of the magnetic field. Among the considered instabilities of azimuthal fields, those of the Chandrasekhar-type, where the background field and the background flow have identical radial profiles, are particularly interesting. -
Exact Two-Dimensionalization of Low-Magnetic-Reynolds-Number
Under consideration for publication in J. Fluid Mech. 1 Exact two-dimensionalization of low-magnetic-Reynolds-number flows subject to a strong magnetic field Basile Gallet1 A N D Charles R. Doering2 1Service de Physique de l’Etat´ Condens´e, DSM, CNRS UMR 3680, CEA Saclay, 91191 Gif-sur-Yvette, France 2Department of Physics, Department of Mathematics, and Center for the Study of Complex Systems, University of Michigan, Ann Arbor, MI 48109, USA (Received 20 April 2021) We investigate the behavior of flows, including turbulent flows, driven by a horizontal body-force and subject to a vertical magnetic field, with the following question in mind: for very strong applied magnetic field, is the flow mostly two-dimensional, with remaining weak three-dimensional fluctuations, or does it become exactly 2D, with no dependence along the vertical? We first focus on the quasi-static approximation, i.e. the asymptotic limit of vanishing magnetic Reynolds number Rm 1: we prove that the flow becomes exactly 2D asymp- totically in time, regardless of the≪ initial condition and provided the interaction parameter N is larger than a threshold value. We call this property absolute two-dimensionalization: the attractor of the system is necessarily a (possibly turbulent) 2D flow. We then consider the full-magnetohydrodynamic equations and we prove that, for low enough Rm and large enough N, the flow becomes exactly two-dimensional in the long- time limit provided the initial vertically-dependent perturbations are infinitesimal. We call this phenomenon linear two-dimensionalization: the (possibly turbulent) 2D flow is an attractor of the dynamics, but it is not necessarily the only attractor of the system. -
Subcritical Magnetohydrodynamic Instabilities: Chandrasekhar's
J. Fluid Mech. (2020), vol. 882, A20. c Cambridge University Press 2019 882 A20-1 doi:10.1017/jfm.2019.841 Subcritical magnetohydrodynamic instabilities: Chandrasekhar's theorem revisited https://doi.org/10.1017/jfm.2019.841 . Kengo Deguchi† School of Mathematics, Monash University, VIC 3800, Australia (Received 10 August 2019; revised 28 September 2019; accepted 14 October 2019) Subcritical instabilities (i.e. finite-amplitude instabilities that occur without any linear instability) in magnetohydrodynamic (MHD) flows are studied by computing finite-amplitude equilibrium solutions of viscous–resistive MHD equations. The plane https://www.cambridge.org/core/terms Couette flow magnetised by a uniform spanwise current is used as a model flow. Solutions are found for broad sub- and super-Alfvénic flow regimes by controlling the magnetic Mach number, but their existence is greatly influenced by the magnetic Prandtl number. When that number is unity, and the walls are perfectly insulating, the solution branch found in the super-Alfvénic regime cannot be continued towards the sub-Alfvénic regime; the boundary between those regimes is called the Chandrasekhar state, where Chandrasekhar (Proc. Natl Acad. Sci. USA, vol. 42, 1956, pp. 273–276) proved the non-existence of a linear ideal instability. Thus, the result may seem to suggest that the Chandrasekhar theorem holds even when diffusivity and nonlinearity are present. This is certainly true, but only when the perturbation magnetic field on the boundary is small. The boundary effects add more complexity to the nonlinear analysis of the Chandrasekhar state. The Chandrasekhar theorem is known to work for flows bounded by perfectly conducting walls. -
Solar Wind Interaction with the Terrestrial Magnetosphere
2002:316 CIV MASTER’S THESIS Solar Wind Interaction with the Terrestrial Magnetosphere LARS G WESTERBERG MASTER OF SCIENCE PROGRAMME Department of Applied Physics and Mechanical Engineering Division of Fluid Mechanics 2002:316 CIV • ISSN: 1402 - 1617 • ISRN: LTU - EX - - 02/316 - - SE SOLAR WIND INTERACTION WITH THE TERRESTRIAL MAGNETOSPHERE Preface This thesis work is done at the Division of Fluid Mechanics, Luleå University of Technology. I would like to thank my supervisor Dr. Hans O. Åkerstedt for his great support and valuable assistance during this project. I would also like to thank all people who have helped and encouraged me throughout the years. i SOLAR WIND INTERACTION WITH THE TERRESTRIAL MAGNETOSPHERE Sammanfattning En studie av strömningen av solvinden kring jordens magnetosfär är gjord. Som förenklad modell används en plan magnetopaus i två dimensioner med stagnationspunkt i ekvatorsplanet. Den teoretiska analysen är gjord genom ordinär störningsräkning. Aktuella samband är härledda ur Navier-Stokes ekvation och MHD ekvationer. En process av speciellt intresse är magnetisk återkoppling. Genom att använda störningsmodellen kan vi göra en analys av gränsskiktet i närhet till den punkt där återkoppling sker. Förutom teoretisk analys används numerisk analys för att lösa partiella differentialekvationer beskrivande strömningen av solvinden kring magnetopausen. Metoden som används är Chebyshev’s kollokationsmetod. Det visar sig att gränsskiktet norr om återkopplingspunkten är tunnare än söder om densamma. Förutsättningen för att stationär återkoppling skall kunna äga rum, är att hastigheten i återkopplingspunkten är mindre än Alfvénhastigheten. Detta får till följd att området kring magnetopausen där vi kan ha stationär återkoppling är begränsat. Hastigheten uppnår Alfvénhastigheten på ett avstånd av ungefär tio jordradier längs magnetopausen. -
Mean-Field Dynamo Model in Anisotropic Uniform Turbulent Flow with Short-Time Correlations
galaxies Article Mean-Field Dynamo Model in Anisotropic Uniform Turbulent Flow with Short-Time Correlations E. V. Yushkov 1,2,3,* , R. Allahverdiyev 4 and D. D. Sokoloff 1,3,5 1 Department of Physics, Lomonosov Moscow State University, Moscow 119991, Russia; [email protected] 2 Space Research Institute RAS (IKI), Moscow 117997, Russia 3 Moscow Center of Fundamental and Applied Mathematics, Moscow 119991, Russia 4 Department of Physics, Moscow State University, Branch in Baku, Baku AZ 1143, Azerbaijan; [email protected] 5 IZMIRAN, Troitsk 142191, Russia * Correspondence: [email protected]; Tel.: +7-(916)-774-52-72 Received: 2 August 2020; Accepted: 14 September 2020; Published: 19 September 2020 Abstract: The mean-field model is one of the basic models of the dynamo theory, which describes the magnetic field generation in a turbulent astrophysical plasma. The first mean-field equations were obtained by Steenbeck, Krause and Rädler for two-scale turbulence under isotropy and uniformity assumptions. In this article we develop the path integral approach to obtain mean-field equations fora short-correlated random velocity field in anisotropic streams. By this model we analyse effects of anisotropy and show the relation between dynamo growth and anisotropic tensors of helicity/turbulent diffusivity. Considering particular examples and comparing results with isotropic cases we demonstrate several mean-field effects: super-exponential growth at initial times, complex dependence of harmonics growth on the helicity tensor structure, when generation is possible for near-zero component or near-zero helicity trace, increase of the averaged magnetic field inclined to the initial current density that leads to effective Lorentz back-reaction and violation of force-free conditions.