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1
Dong, Chuanfei. "Heating of ions by low-frequency Alfven waves in solar atmosphere". Thesis, Georgia Institute of Technology, 2010. http://hdl.handle.net/1853/37160.
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The exact mechanisms responsible for heating the solar atmosphere in regions such as the chromosphere (partially ionized) and the corona (fully ionized) remain quantitatively unknown. This thesis demonstrates that the ions can be heated by Alfven waves with low frequencies in fully and partially ionized low beta plasmas, which is contrary to the customary expectation. For the partially ionized case, we find the heating process to be less efficient than the scenario with no ion-neutral collisions, and that the heating efficiency depends on the ratio of ion-neutral collision frequency to the ion gyrofrequency. For Alfven waves propagating obliquely to the background magnetic field in fully ionized plasmas, we find the heating process to be more efficient than the situation with Alfven waves propagating along the background magnetic field. Furthermore, the simulation results show the parallel kinetic temperature can become even larger than the perpendicular component for the case of obliquely propagating Alfven waves.
2
Betti, Riccardo. "Kinetic effects on global Alfvén waves". Thesis, Massachusetts Institute of Technology, 1991. http://hdl.handle.net/1721.1/32129.
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Compton, Christopher S. "Propagation of Alfvén waves in the WVU HELIX device". Morgantown, W. Va. : [West Virginia University Libraries], 2006. https://eidr.wvu.edu/etd/documentdata.eTD?documentid=4525.
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Thesis (M.S.)--West Virginia University, 2006.Title from document title page. Document formatted into pages; contains iv, 22 p. : ill. (some col.). Includes abstract. Includes bibliographical references (p. 22).
4
Ivchenko, Nickolay. "Alfven Waves and Spatio-Temporal Structuring in the Auroral Ionosphere". Doctoral thesis, KTH, Alfvénlaboratoriet, 2002. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-3364.
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5
Pinches, Simon David. "Nonlinear interaction of fast particles with Alfven waves in tokamaks". Thesis, University of Nottingham, 1996. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.362917.
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6
Manrique, Marcos Antonio Albarracin. "Plasma Diasnostic in Tokamaks Using Alfvén Waves". Universidade de São Paulo, 2015. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-14082015-110334/.
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In this work we investigated the excitation of Alfvén eigenmodes in tokamaks using external antennas to the plasma column. The basic theory of Alfvén waves is revised, including non-ideal effects such as resistivity. Then the theoretical model for excitation Alfvén waves in a cylindrical plasma column, developed by Kurt Appert, is shown in detail, as an introduction to the more complex problem of Alfvén waves in toroidal plasmas. The cylindrical model is implemented in a numerical code, which is used to study the excitation of Global Alfvén Waves (GAWs), below to the so-called Continuum of Alfvén, in TCABR and JET tokamaks, using a realistic description of their antenna systems. In the sequel, it is given a brief description of Toroidal Alfvén eigenmodes (TAEs) that are excited in the gaps of the Continuum of Alfvén created by the periodicity condition of the toroidal configuration. The excitement of these modes in JET tokamak is studied using the codes HELENA, for reconstruction of magneto-hydrodynamic equilibrium, and CASTOR, which calculates the perturbed fields in this equilibrium, coupled with instability or modes excited within the magneto-resistive hydrodynamic model. This study was carried out in order to determine, consistently, the spectrum quality and the eigenmodes associated with TAEs, with different numbers toroidal n, excited by the new JET antenna system. In particular, it was investigated in detail the effect of the phases of the supply currents of the different modules (eight) of the antenna system in the quality of the excited spectrum, using an original method, implemented in this work, based on the CASTOR code. The results indicate that, although the excitation of a certain mode may be a privileged by an optimized choice of phases, satellite modes can also be excited with higher amplitude, so that the purity of the spectrum is not substantially improved. This is the main result obtained in this work.Neste trabalho é investigada a excitação de modos própios de Alfvén em tokamaks, utilizando antenas externas à coluna de plasma. A teoria básica das ondas de Alfvén é revista, incluindo efeitos não ideais, como resistividade. A seguir, o modelo teórico para excitação de ondas de Alfvén numa coluna cilindrica de plasma, desenvolvido por Kurt Appert, é apresentado em detalhe, como introdução ao problema mais complexo de ondas de Alfvén em plasmas toroidais. O modelo cilindrico é implementado em um código numérico, que é utilizado para estudar a excitação de modos globais de Alfvén (GAWs - Global Alfvén Waves), abaixo do chamado Continuo de Alfvén, nos tokamaks TCABR e JET, utilizando uma descrição realista de seus sistemas de antenas. A seguir é feita uma breve descrição dos auto modos toroidais de Alfvén (TAEs - Toroidal Alfvén Eigenmodes) que são excitados nas brechas do Continuo de Alfvén criadas pela condição de periodicidade em configurações toroidais. A excitação desses modos no tokamak JET é estudada utilizando os códigos HELENA, para reconstrução do equilíbrio magneto-hidrodinâmico, e CASTOR, que calcula os campos perturbados nesse equilíbrio, associados a instabilidades ou modos excitados, dentro do modelo magneto-hidrodinâmico resistivo. Esse estudo foi feito com o objetivo de determinar, de forma consistente, a qualidade do espectro e as auto-funções associadas a TAEs, com diferentes números toroidais n, excitados pelo atual sistema de antenas do JET. Em particular, foi investigado em detalhe o efeito das fases das correntes de alimentação dos diferentes módulos (oito) do sistema de antenas na qualidade do espectro excitado, utilizando um método original, implementado neste trabalho, de utilizar o código CASTOR. Os resultados indicam que embora a excitação de um determinado modo possa ser privilegiado por uma escolha ótima das fases, modos satélites também podem ser excitados com maior amplitude, de modo que a pureza do espectro não é substancialmente melhorada. Este é o principal resultado obtido neste trabalho.
7
Cox, Grace Alexandra. "Torsional Alfvén waves in the Earth's core". Thesis, University of Leeds, 2015. http://etheses.whiterose.ac.uk/9973/.
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Torsional Alfvén waves are theoretically predicted to exist in Earth's outer core, have been inferred from geophysical data and observed in geodynamo simulations. They provide an indirect means of investigating core dynamics, core properties and core-mantle coupling mechanisms. In this study, we produce 1-D forward models of torsional waves in Earth's core and study the wave-induced secular variation (SV). We find that torsional waves undergo significant dispersion during propagation that arises due to their geometric setting, with long wavelength features being more dispersive than short wavelength features. Other key propagation features observed in our models are phase shifts at Earth's rotation axis, low amplitude wakes trailing behind sharply defined pulses, reflections from the tangent cylinder and internal wave reflections caused by strong magnetic field gradients. These combined dispersive effects may lead to difficulties in resolving the excitation mechanism of any torsional waves identified in geophysical data. Fast torsional waves with amplitudes and timescales consistent with a recent study of the 6 yr Δ LOD signal (Gillet et al., 2010) induce very rapid, small (maximum ~2 nT/yr at Earth's surface) SV signals that likely could not be resolved in observations of the Earth's SV. Slow torsional waves with amplitudes and timescales consistent with, for example, Zatman & Bloxham (1997), Hide et al. (2000) produce larger SV signals that reach amplitudes of ~20 nT/yr at Earth's surface. We applied the two-part linear regression jerk detection method developed by Brown et al. (2013) to the SV induced by slow torsional waves, using the same parameters as used on real SV, which identified several synthetic jerk events. As the local magnetic field morphology dictates which regions are sensitive to zonal core flow, and not all regions are sensitive at the same time, the modelled waves are not able to induce global contemporaneous jerk events such as that observed in 1969. The synthetic jerks are only observed on regional scales and generally occur in a single SV component. Also, the identified events are periodic due to waves passing beneath locations periodically and the SV signals are smoothly varying. These smooth signals are more consistent with the geomagnetic jerks envisaged by Demetrescu & Dobrica (2005, 2014), than the sharp 'V' shapes that are typically associated with geomagnetic jerks.
8
Patrick, Antolin Tobos. "Predicting observational signatures of coronal heating by Alfven waves and nanoflares". 京都大学 (Kyoto University), 2009. http://hdl.handle.net/2433/126571.
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Kyoto University (京都大学)0048
新制・課程博士
博士(理学)
甲第14894号
理博第3463号
新制||理||1507(附属図書館)
27332
UT51-2009-M808
京都大学大学院理学研究科物理学・宇宙物理学専攻
(主査)教授 柴田 一成, 教授 一本 潔, 教授 嶺重 慎
学位規則第4条第1項該当
9
Khotyaintsev, Yuri. "Alfvén Waves and Energy Transformation in Space Plasmas". Doctoral thesis, Uppsala universitet, Institutet för rymdfysik, Uppsalaavdelningen, 2002. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-3264.
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This thesis is focused on the role of Alfvén waves in the energy transformation and transport in the magnetosphere. Different aspects of Alfvén wave generation, propagation and dissipation are considered. The study involves analysis of experimental data from the Freja, Polar and Cluster spacecraft, as well as theoretical development. An overview of the linear theory of Alfvén waves is presented, including the effects of fnite parallel electron inertia and fnite ion gyroradius, and nonlinear theory is developed for large amplitude Alfvén solitons and structures. The methodology is presented for experimental identification of dispersive Alfvén waves in a frame moving with respect to the plasma, which facilitates the resolution of the space-time ambiguity in such measurements. Dispersive Alfvén waves are identified on field lines from the topside ionosphere up to the magnetopause and it is suggested they play an important role in magnetospheric physics. One of the processes where Alfvén waves are important is the establishment of the field aligned current system, which transports the energy from the reconnection regions at the magnetopause to the ionosphere, where a part of the energy is dissipated. The main mechanism for the dissipation in the top-side ionosphere is related to wave-particle interactions leading to particle energization/heating. An observed signature of such a process is the presence of parallel energetic electron bursts associated with dispersive Alfvén waves. The accelerated electrons (electron beams) are unstable with respect to the generation of high frequency plasma wave modes. Therefore this thesis also demonstrates an indirect coupling between low frequency Alfvén wave and high frequency oscillations.
10
Martin, Clare E. "Alfvén waves in low-mass star-forming regions". Thesis, University of St Andrews, 1999. http://hdl.handle.net/10023/14190.
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Low-mass star-forming regions have a lifetime which is greater than their dynamical time and must therefore be, in an average sense, in mechanical equilibrium. The work presented here proposes that an equilibrium exists between the self-gravity, gas pressure, and the magnetic field and the waves it supports. Specifically the equilibrium in the direction perpendicular to the ordered magnetic field is given by the Lorentz force, while that parallel to the field is given by an Alfvén wave pressure force. The work detailed in this thesis models a low-mass star-forming region as a one-dimensional gas slab with a magnetic field lying perpendicular to the layer. Analytical, self-consistent models are formulated to study the equilibrium parallel to the background magnetic field. It is found that both short-wavelength (modelled using the WKB approximation) and large-amplitude, long-wavelength Alfvén waves can provide the necessary support parallel to the magnetic field, generating model cloud thicknesses that are consistent with the observations. The effect of damping by the linear process of ion-neutral friction is considered. It is found that the damping of the waves is not a necessary condition for the support of the cloud although it is an advantage. The possible sources of these waves are discussed. The Alfvén waves are also found to make an important contribution to the heating of a low-mass star-forming region. By modelling the dominant heating and cooling mechanisms in a molecular cloud, it is discovered that a cloud supported against its self-gravity by short-wavelength Alfvén waves will be hotter at its outer edge than in the central regions. These models successfully describe a low-mass star-forming region in equilibrium between its self-gravity, the gas pressure and an Alfvén wave pressure force. The question of the stability of such an equilibrium is considered, specifically that of an isothermal gas slab supported by short-wavelength Alfvén waves. The initial results suggest that the presence of a magnetic field and its associated Alfvén waves have a stabilising effect on the layer, and encourage further consideration of the role of Alfvén waves in low-mass star-forming regions.
11
Russell, Alexander J. B. "Coupling of the solar wind, magnetosphere and ionosphere by MHD waves". Thesis, University of St Andrews, 2010. http://hdl.handle.net/10023/2571.
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The solar wind, magnetosphere and ionosphere are coupled by magnetohydrodynamic waves, and this gives rise to new and often unexpected behaviours that cannot be produced by a single, isolated part of the system. This thesis examines two broad instances of coupling: field-line resonance (FLR) which couples fast and Alfvén waves, and magnetosphere-ionosphere (MI-) coupling via Alfvén waves. The first part of this thesis investigates field-line resonance for equilibria that vary in two dimensions perpendicular to the background magnetic field. This research confirms that our intuitive understanding of FLR from 1D is a good guide to events in 2D, and places 2D FLR onto a firm mathematical basis by systematic solution of the governing equations. It also reveals the new concept of ‘imprinting’ of spatial forms: spatial variations of the resonant Alfvén wave correlate strongly with the spatial form of the fast wave that drives the resonance. MI-coupling gives rise to ionosphere-magnetosphere (IM-) waves, and we have made a detailed analysis of these waves for a 1D sheet E-region. IM-waves are characterised by two quantities: a speed v_{IM} and an angular frequency ω_{IM} , for which we have obtained analytic expressions. For an ideal magnetosphere, IM-waves are advective and move in the direction of the electric field with speed v_{IM}. The advection speed is a non-linear expression that decreases with height-integrated E-region plasma-density, hence, wavepackets steepen on their trailing edge, rapidly accessing small length-scales through wavebreaking. Inclusion of electron inertial effects in the magnetosphere introduces dispersion to IM-waves. In the strongly inertial limit (wavelength λ << λ_{e} , where λ_{e} is the electron inertial length at the base of the magnetosphere), the group velocity of linear waves goes to zero, and the waves oscillate at ω_{IM} which is an upper limit on the angular frequency of IM-waves for any wavelength. Estimates of v_{IM} show that this speed can be a significant fraction (perhaps half) of the E_{⊥} × B_{0} drift in the E-region, producing speeds of up to several hundred metres per second. The upper limit on angular frequency, ωIM , is estimated to give periods from a few hundredths of a second to several minutes. IM-waves are damped by recombination and background ionisation, giving an e-folding decay time that can vary from tens of seconds to tens of minutes. We have also investigated the dynamics and steady-states that occur when the magnetosphere-ionosphere system is driven by large-scale Alfvénic field-aligned currents. Steady-states are dominated by two approximate solutions: an ‘upper’ solution that is valid in places where the E-region is a near perfect conductor, and a ‘lower’ solution that is valid where E-region depletion makes recombination negligible. These analytic solutions are extremely useful tools and the global steady-state can be constructed by matching these solutions across suitable boundary-layers. Furthermore, the upper solution reveals that E-region density cavities form and widen (with associated broadening of the magnetospheric downward current channel) if the downward current density exceeds the maximum current density that can be supplied by background E-region ionisation. We also supply expressions for the minimum E-region plasma-density and shortest length-scale in the steady-state. IM-waves and steady-states are extremely powerful tools for interpreting MI-dynamics. When an E-region density cavity widens through coupling to an ideal, single-fluid MHD magnetosphere, it does so by forming a discontinuity that steps between the upper and lower steady-states. This discontinuity acts as part of an ideal IM-wave and moves in the direction of the electric field at a speed U = \sqrt{v_{IM} {+} v_{IM} {-}}, which is the geometric mean of v_{IM} evaluated immediately to the left and right of the discontinuity. This widening speed is typically several hundreds of metres per second. If electron inertial effects are included in the magnetosphere, then the discontinuity is smoothed, and a series of undershoots and overshoots develops behind it. These undershoots and overshoots evolve as inertial IM-waves. Initially they are weakly inertial, with a wavelength of about λ_{e}, however, strong gradients of ω_{IM} cause IM-waves to phase-mix, making their wavelength inversely proportional to time. Therefore, the waves rapidly become strongly inertial and oscillate at ω_{IM}. The inertial IM-waves drive upgoing Alfvén waves in the magnetosphere, which populate a region over the downward current channel, close to its edge. In this manner, the E-region depletion mechanism, that we have detailed, creates small-scale Alfvén waves in large-scale current systems, with properties determined by MI-coupling.
12
Brugman, Brian Thomas. "An investigation of the nonlinear interaction of Alfvén waves". Diss., Restricted to subscribing institutions, 2007. http://proquest.umi.com/pqdweb?did=1459917811&sid=1&Fmt=2&clientId=1564&RQT=309&VName=PQD.
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Schäfer, Sebastian. "Spatial and temporal structure of Alvén resonator waves at the terrestrial Plasmapause". [Katlenburg-Lindau] Copernicus Publ, 2008. http://d-nb.info/993339034/04.
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14
Verwichte, Erwin Andre Omer. "Aspects of nonlinearity and dissipation in magnetohydrodynamics". Thesis, Open University, 1999. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.326565.
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Simpson, David. "Absolute and convective instabilities of circularly polarized AlfveÌn waves". Thesis, University of Sheffield, 2005. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.425186.
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Nielson, Kevin Derek. "Analysis and gyrokinetic simulation of MHD Alfvén wave interactions". Diss., University of Iowa, 2012. https://ir.uiowa.edu/etd/3504.
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The study of low-frequency turbulence in magnetized plasmas is a difficult problem due to both the enormous range of scales involved and the variety of physics encompassed over this range. Much of the progress that has been made in turbulence theory is based upon a result from incompressible magnetohydrodynamics (MHD), in which energy is only transferred from large scales to small via the collision of Alfv ́n waves propagating oppositely along the mean magnetic field. Improvements in laboratory devices and satellite measurements have demonstrated that, while theories based on this premise are useful over inertial ranges, describing turbulence at scales that approach particle gyroscales requires new theory.
In this thesis, we examine the limits of incompressible MHD theory in describing collisions between pairs of Alfvén waves. This interaction represents the fundamental unit of plasma turbulence. To study this interaction, we develop an analytic theory describing the nonlinear evolution of interacting Alfv ́n waves and compare this theory to simulations performed using the gyrokinetic code AstroGK. Gyrokinetics captures a much richer set of physics than that described by incompressible MHD, and is well-suited to describing Alfvénic turbulence around the ion gyroscale. We demonstrate that AstroGK is well suited to the study of physical Alfvén waves by reproducing laboratory Alfvén dispersion data collected using the LAPD. Additionally, we have developed an initialization alogrithm for use with AstroGK that allows exact Alfvén eigenmodes to be initialized with user specified amplitudes and phases.
We demonstrate that our analytic theory based upon incompressible MHD gives excellent agreement with gyrokinetic simulations for weakly turbulent collisions in the limit that k⊥ ρi << 1. In this limit, agreement is observed in the time evolution of nonlinear products, and in the strength of nonlinear interaction with respect to polarization and scale. We also examine the effect of wave amplitude upon the validity of our analytic solution, exploring the nature of strong turbulence. In the kinetic limit where k⊥ ρi ≥ 1 where incompressible MHD is no longer a valid description, we illustrate how the nonlinear evolution departs from our analytic expression.
The analytic theory we develop provides a framework from which more sophisticated of weak and strong inertial-range turbulence theories may be developed. Characterization of the limits of this theory may provide guidance in the development of kinetic Alfvén wave turbulence.
17
Schroeder, James William Ryan. "Exploring the Alfvén-wave acceleration of auroral electrons in the laboratory". Diss., University of Iowa, 2017. https://ir.uiowa.edu/etd/5846.
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Inertial Alfvén waves occur in plasmas where the Alfvén speed is greater than the electron thermal speed and the scale of wave field structure across the background magnetic field is comparable to the electron skin depth. Such waves have an electric field aligned with the background magnetic field that can accelerate electrons. It is likely that electrons are accelerated by inertial Alfvén waves in the auroral magnetosphere and contribute to the generation of auroras. While rocket and satellite measurements show a high level of coincidence between inertial Alfvén waves and auroral activity, definitive measurements of electrons being accelerated by inertial Alfvén waves are lacking. Continued uncertainty stems from the difficulty of making a conclusive interpretation of measurements from spacecraft flying through a complex and transient process. A laboratory experiment can avoid some of the ambiguity contained in spacecraft measurements.
Experiments have been performed in the Large Plasma Device (LAPD) at UCLA. Inertial Alfvén waves were produced while simultaneously measuring the suprathermal tails of the electron distribution function. Measurements of the distribution function use resonant absorption of whistler mode waves. During a burst of inertial Alfvén waves, the measured portion of the distribution function oscillates at the Alfvén wave frequency. The phase space response of the electrons is well-described by a linear solution to the Boltzmann equation. Experiments have been repeated using electrostatic and inductive Alfvén wave antennas. The oscillation of the distribution function is described by a purely Alfvénic model when the Alfvén wave is produced by the inductive antenna. However, when the electrostatic antenna is used, measured oscillations of the distribution function are described by a model combining Alfvénic and non-Alfvénic effects. Indications of a nonlinear interaction between electrons and inertial Alfvén waves are present in recent data.
18
Voronkov, Igor. "Shear Alfvén waves and shear flow instabilities in the Earth's magnetosphere". Thesis, National Library of Canada = Bibliothèque nationale du Canada, 1998. http://www.collectionscanada.ca/obj/s4/f2/dsk2/tape15/PQDD_0003/NQ34851.pdf.
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Lilley, Matthew Keith. "Resonant interaction of fast particles with Alfvén waves in spherical tokamaks". Thesis, Imperial College London, 2009. http://hdl.handle.net/10044/1/5487.
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The Spherical Tokamak (ST) concept has become one of the main avenues in magnetic nuclear fusion research since STs successfully demonstrated plasma operation at [Beta] = 2P[mu]0=B2~1. Next step ST machines aiming at achieving burning plasma conditions in high [Beta] plasmas are being planned, such as the Spherical Tokamak Power Plant (STPP) and the Component Testing Facility (CTF). Instabilities of fast particle-driven Alfven eigenmodes are often observed in present-day STs. Such instabilities, driven by fusion-born alpha particles as well as by fast ions produced with auxiliary heating schemes, in the next step STs may pose a major problem as these instabilities may affect confinement and losses of the fast ions. A theory of compressional Alfven eigenmodes (CAE) with frequencies above the deuterium cyclotron frequency,[omega] > [omega]cD, is developed for plasma parameters of a STPP, and modes in the ion-ion hybrid frequency range, [omega]cT < [omega] < [omega]cD, are also investigated in order to assess the potential of diagnosing the deuterium-tritium (D-T) ratio. For the 1-D character of a STPP equilibrium with [Beta]~1 , a `hollow cylinder' toroidal plasma model is employed for studying CAEs with arbitrary values of the parallel wave-vector k[||] = k[.]B/|B|. The existence of weakly-damped CAEs, free of mode conversion, is shown to be associated with the `well' in the magnetic field profile, B = B (R), that can exist at the magnetic axis. A significant part of this thesis focusses on the experimentally observed effects of resonant wave-particle interaction between Alfven waves and fast particles in the Mega Amp Spherical Tokamak (MAST) device at the Culham Laboratory, UK, and in the LArge Plasma Device (LAPD) in the University of California, Los-Angeles, USA. New robust experimental scenarios for exciting CAEs in the MAST spherical tokamak are developed, and interpretation of the observed CAEs in the frequency range [omega]cD/3 < [omega] < [omega]cD is given in the context of the 1-D ST model and the Doppler shifted cyclotron resonance. The e ciency of the Doppler resonance between co and counter directed fast ions and left and right hand polarised Alfven waves is further assessed experimentally on the LAPD device, with probe ions injected in the presence of Alfv en waves launched by an external antenna. The developed theory of CAEs is then applied to a calculation of the linear kinetic drive of CAEs in the MAST experiments. A model representation of the fast ion distribution function, produced by neutral beam injection (NBI), is used by fitting to the TRANSP Monte-Carlo NBI modelling results. The main free energy sources associated with temperature anisotropy and bump-on-tail are estimated analytically, and the CAE stability boundary is qualitatively assessed. In order to explain the experimentally observed difference between steady-state and pulsating Alfvenic modes, the non-linear theory of fast particle driven modes near marginal stability is extended to include dynamical friction (drag). For the bump-on-tail problem, the drag is shown to always give an explosive amplitude evolution in contrast to diffusion in velocity space in the vicinity of the wave-particle resonance. This is then extended to the case of experimentally observed NBI-driven toroidal Alfven eigenmodes (TAEs) in the MAST machine. The experimentally observed differences between TAEs driven by fast ions produced with ion cyclotron resonance heating (ICRH) and NBI are then interpreted. The problem of drag dominated collisions for modes excited by fusion-born alpha particles in burning plasmas such as a STPP and ITER is underlined.
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Matsumoto, Takuma. "Spicule Formation, Coronal Heating, and Solar Wind Acceleration with Alfven waves driven by observed photospheric motions". 京都大学 (Kyoto University), 2010. http://hdl.handle.net/2433/120664.
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Shigueoka, Hisataki. "Estudo espectral das ondas de Alfvén em plasma cilíndrico". Universidade de São Paulo, 1991. http://www.teses.usp.br/teses/disponiveis/43/43131/tde-04092012-113407/.
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Neste trabalho foi estudado o espectro das ondas de MHD ideal em um plasma cilíndrico. Considerando o plasma inomogêneo, o espectro apresenta regiões discretas e contínuas: onda lenta e onda de Alfvén. Os automodos das regiões discretas são as soluções da equação de Hain-Lüst e, nas regiões contínuas, as autofunções apresentam singularidades. Foram determinadas expressões analíticas em termos da função de Bessel que os autovalores da onda de Alfvén apresentam o comportamento discreto. Os modos globais discretos de Alfvén foram calculados usando um equilíbrio da configuração de tokamak, beta < 1, e estes modos apresentam uma pequena contribuição da onda compressional. Foi feita uma análise da propagação da energia da onda por meio do vetor de Poynting e este conhecimento tem a sua importância no problema de aquecimento do plasma por ondas de Alfvén. Foi feita, também, uma análise da polarização das ondas. Foi estudado o espectro da onda devido ao efeito de beta, beta > 1. Esta condição é mais aplicável em problemas de plasma espacial, por exemplo, na fotosfera solar. Foram obtidos, pela primeira vez, os modos discretos de onda lenta, previstos teoricamente. As suas soluções (autofunções e autovalores) possuem também a característica global, aqui denominadas de modos globais discretos da onda lenta. Outro estudo do problema espectral foi realizado para urna configuração de equilíbrio para RFP (\"Reversed Field Pinch\"). Determinou-se, além dos automodos Sturmianos da onda de Alfvén, os automodos anti-Sturmianos da onda lenta.The spectrum of the ideal MHD waves in cylindrical plasmas has been studied. Assuming non homogeneous plasma, the spectrum presents the discrete and continuum (slow and Alfvén waves) regions. The eigenfunctions of the discrete regions are the solutions of the Hain-Lüst equation. In the continua, the solutions of this equation have singularities. It has been determined analytical expressions for the discrete eigenfunctions. These happen to be the Bessel\'s function and its eigenvalues agree with the numerical calculations. The discrete modes (global modes) of Alfvén waves have been calculated by numerically using the equilibrium configuration of tokamaks, beta < 1, and it was observed that these modes present a small contribution from the compressional waves. An analysis of the energy propagation was done using the Poynting vector. This has its importance in the problem of plasma heating by Alfvén waves. Its polarization was also studied. The effect of beta, through values greater than 1, was also studied. This condition is more aplicable to the spacial plasma problems, for example, in the solar photosphere\'s plasma. It has been calculated, for the first time, the discrete modes of slow waves, proposed theoretically. Its solutions (eigenfunctions and eigenvalues) have also the characteristics of the global modes, called global discrete slow waves. The study of spectral problems for the Reversed Field Pinch configurations was also determined here for both Sturmian eigenmodes for the Alfvén waves and Anti-Sturmian eigenmodes for the slow waves.
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Thuecks, Derek Jon. "Laboratory investigations of dispersive Alfvén waves and their role in electron acceleration". Diss., University of Iowa, 2009. https://ir.uiowa.edu/etd/268.
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Two sets of related experiments are presented here. In the first, measurements of shear Alfvén waves are used to test the predictions of a variety of different electron collision operators, including several Krook collision operators as well as a Lorentz collision operator. New expressions for the collisional warm-plasma dielectric tensor resulting from the use of the fully-magnetized collisional Boltzmann equation are presented here. Theoretical predictions for the parallel phase velocity and damping as a function of perpendicular wave number k⊥ are derived from the dielectric tensor. Laboratory measurements of the parallel phase velocity and damping of shear Alfvén waves were made to test these theoretical predictions in both the kinetic (vte ≫ vA) and inertial (vte ≪ vA) parameter regimes and at several wave frequencies (ω < ωci). Results show that in the inertial regime, the best match between measurements and theory occur when any of the Krook operators are used to describe electron collisions. In contrast, the best agreement in the kinetic regime is found when collisions are completely ignored.
In the second set of experiments, whistler waves were launched and received by a pair of dipole antennas immersed in the plasma at two positions along the background magnetic field. According to cold-plasma theory, there is absorbtion of the whistler wave when ω = |ωce| = eB/me due to resonance with the electrons. The whistler frequency was swept from somewhat below up to the electron cyclotron frequency |ωce|. As the frequency was swept, the wave was resonantly absorbed by those parts of electron phase space density which were Doppler shifted into resonance. The transmission of the wave through the plasma was measured. This measurement of transmission can be converted into a measure of the parallel electron distribution function. This diagnostic is designed to attempt to measure modifications to the parallel electron distribution function due to interactions with inertial Alfvén waves.
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Feher, Tamas Bela [Verfasser]. "Simulation of the interaction between Alfvén waves and fast particles / Tamas Bela Feher". Greifswald : Universitätsbibliothek Greifswald, 2014. http://d-nb.info/1048536556/34.
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Ozeke, Louis Godwin. "Modelling the generation and properties of guided AlfveÌn waves in the magnetosphere". Thesis, University of York, 2002. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.273889.
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Puglia, Paulo Giovane Paschoali Pereira. "Excitação de ondas de helicon e de Alfvén em tokamak TCABR". Universidade de São Paulo, 2011. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-30092011-155130/.
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O objetivo do trabalho é a investigação da excitação de ondas no plasma com o uso de uma antena externa e fazer uma análise das ressonâncias de Alfvén encontradas. O sistema de antenas de Alfvén no tokamak TCABR foi desenhado para aquecimento do plasma por meio de ressonâncias. Al em do aquecimento, é possível usar a detecção de ondas excitadas com o uso da antena para objetivos de diagnóstico do plasma, encontrando o valor do perfil de segurança e massa efetiva dos íons. Por causa de uma falha nos diodos do campo toroidal usamos o regime de disparos de limpeza, com campo magnético toroidal mais fraco que de disparos tópicos do TCABR, para os testes do método de excitação e identificação de ressonâncias no plasma. Com o uso do circuito demodulador foram medidas ondas de helicon excitadas com a antena de Alfvén no plasma de limpeza usando as sondas magnéticas e de Langmuir. Com simulação foi possível idênticas as ondas medidas. Há disponível um gerador de frequência variável que foi utilizado junto desse experimento. Ambos os equipamentos se encontram preparados para uso, sendo a próxima etapa usar o plasma tópico de disparo do TCABR, que tem maior densidade que o plasma de limpeza. As medidas realizadas foram um teste para o circuito demodulador e gerador de frequência variável, que teve seu comportamento comparado com os dados de um osciloscópio de alta frequência de amostragem. Os equipamentos do TCABR usados nos experimentos, as antenas e sondas magnéticas, um gerador de baixa potência com frequência variável, um circuito demodulador, sonda de Langmuir e o reflectômetro, que tem alta taxa de amostragem (200MHz) e varredura de frequência na banda de 18 40GHz. São todos descritos na dissertação. Para modelagem das ressonâncias de Alfvén foi feito o cálculo do tensor dielétrico do plasma para o modelo cinético e para o limite magnetohidrodinâmico. Por meio de simulação computacional e cálculos considerando plasma como um fluido de 2 componentes, no caso prótons e elétrons, é possível determinar alguns tipos de onda que podem ser excitadas no plasma e sua relação de dispersão, foram calculadas a onda magnetossônica rápida e a onda global de Alfvén. Determinamos radialmente a posição dos campos eletromagnéticos no plasma. Usando o reactômetro foram medidas as ressonâncias das ondas de Alfvén na borda do plasma induzidas pelas antenas, com o plasma tópico do tokamak, com densidade mais alta e o gerador de alta potência com frequência fixa. O método para achar as ressonâncias nos dados do reflectômetro foi com o uso de sidebands que aparecem em torno da frequência da ressonância não sinal do reflectômetro, que é a frequência do gerador. As sidebands foram analisadas com um espectrograma dos dados. As ondas excitadas na borda do plasma puderam ser identificadas também nas simulações. Os resultados da análise mostram que foi possível medir as ondas no plasma que foram excitadas com o uso das antenas e tanto o circuito demodulador com o uso de sondas magnéticas como o reflectômetro são adequados para se achar ressonâncias no plasma.The objective of this work is to investigate the excitation of waves in a plasma using an antenna and to analyse the Alfvén resonances found. The Alfvén antenna heating system of the TCABR tokamak was designed to heat the plasma due to resonances. As the diodes of the toroidal field had burned down we used cleaning discharges, with low toroidal magnetic field, to test the excitation method and the identification of plasma resonances. With the demodulator circuit we measured helicon waves excited with the Alfv en antenna in the cleaning plasma using Langmuir and magnetic probes. With computational simulation we found the measured waves. A generator of variable frequency was used in this experiment. Both equipments are prepared for future experiments with the typical plasma of the TCABR, which has higher density than the cleaning plasma. This work was aimed to test to the demodulator circuit and the variable frequency generator, the data obtained were compared to that of a high sampling frequency oscilloscope. It is presented the description of the TCABR equipments used, antenna, magnetic probe, variable frequency generator of low power, demodulator circuit, Langmuir probe and a reflectometer which has a high sampling frequency (200MHZ) and frequency scanning in the range 18 40GHz, and was built in Portugal. In order to have a model of Alfv en resonances we calculated the plasma dieletric tensor both in the kinetic and magnetohydrodynamic limits. With computational simulation and using a two uid model, protons and electrons, it is possible to find some of the excited waves in the plasma and its dispersion relation, we calculated the fast magnetosonic wave and the global Alfvén wave. We found the radial position of the electromagnetic fields in the plasma. With the re ectometer we measured resonances of Alfvén waves induced by the antenna at the plasma border in a typical TCABR tokamak plasma discharge, with higher density and a high power fixed frequency generator. We used sidebands as a method to find out the resonances in the reflectometer data. These sidebands are localized around the resonance frequency, which is the Alfvén wave generator frequency. The sidebands were analysed with spectrograms of the data. The waves excited at the plasma border were also found in the simulation. The analysis results show that we could detect the plasma waves excited with the antennas. The demodulator circuit along with magnetic probes and the reflectometer can be used to find plasma resonances.
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Guidolin, Luiz Carlos Büttner Mostaço. "Determinação da configuração de ondas de alfvén excitadas no tokamak TCABR". Universidade de São Paulo, 2007. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-23042009-230419/.
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Para o aprimoramento do sistema de aquecimento do plasma por meio de ondas de Alfvén, denominado sistema AWES Alfvén Waves Excitment System, do tokamak TCABR foram construídos, caracterizados, instalados e colocados em operação os diagnósticos para determinação da potência de rádio-freqüência fornecida ao plasma pelo conjunto de antenas para excitação de ondas de Alfvén bem como o circuito processador de sinais para o conjunto de sondas magnéticas, já instaladas dentro da câmara do TCABR, que permitem determinar o espectro de rádio-freqüência gerado pelo conjunto de antenas no interior da câmara de vácuo deste tokamak. Cada conjunto do sistema de diagnóstico de potência é composto por três dispositivos, sendo eles, um sensor de corrente de rádio-freqüência, do tipo bobinas de Rogowski, um sensor de tensão de RF, composto de divisores de tensão acoplados a um circuito processador de sinais e por um circuito multiplicador de sinais capaz de multiplicar os sinais de corrente e tensão de RF e fornecer um sinal proporcional à potência efetivamente fornecida ao plasma. No total foram construídas dez bobinas de Rogowski cujas constantes de sensibilidade são da ordem de 18 mV/A, doze divisores de tensão capazes de reduzir a amplitude de um sinal de 10kV a aproximadamente 5V, seis circuitos processadores de sinais para determinação da tensão de RF e quatro multiplicadores de sinais. Além disso foi construído um circuito processador de sinais capaz de processar o sinal fornecido por quatro sondas magnéticas simultaneamente. Todos os dispositivos elaborados nesse trabalho são capazes de processar sinais de freqüências compreendidas na faixa de 3 a 6MHz e fornecer sinais de baixa freqüência tal que seja possível adquiri-los automaticamente pelo sistema de aquisição de dados do TCABR, denominado TCAqs. Para os procedimentos de calibração e testes de funcionamento dos equipamentos desenvolvidos neste trabalho, estabeleceu-se um Sistema de Calibração Automatizado (SCA) sendo uma de suas partes integrantes um software capaz de comunicar e controlar equipamentos de medição, tais como osciloscópios e geradores de sinais, através de portas de comunicação tipo RS-232 usando a linguagem de comunicação SCPI. Este programa, chamado de SCO, foi inteiramente desenvolvido em software livre e de código aberto para ser usado em sistemas operacionais Unix-Like, como os sistemas GNU/Linux. O código fonte do SCO foi liberado como software livre e com isso registrado sob a licença GNU/GPL. Os procedimentos de calibração uma vez operando sob esse sistema cuja principal característica é a funcionalidade de automação, permitiu a aquisição de uma quantidade de dados muito maior do que aquela que seria possível em procedimentos manuais, resultando assim, em curvas mais confiáveis do ponto de vista estatístico aumentando-se conseqüentemente, de forma considerável, a qualidade das medições. Após extensa caracterização e testes de funcionamento fora e no TCABR concluiu-se que estes dispositivos estão prontos para serem utilizados em campanhas experimentais.In order to enhance the efficiency of the TCABR\'s Alfvén waves heating system, called AWES - Alfvén Waves Excitement System a diagnostics for determining the radio-frequency power applied to the plasma and a processing circuit for the magnetic coil system was built, characterized, installed and put into operation. The RF diagnostics system was designed to determine the total power that the set of AWES antennas applies to the plasma and, the magnetic coils system is designed to determine the RF spectrum excited by these antennas. Since the magnetic coils are already installed inside the TCABRs vacuum chamber only the signal processing circuit was built for it. The RF power diagnostics set is composed of three devices which are, one RF current sensing device, a set for determining the RF voltage and a multiplying system. A Rogowski coil is used for measuring the RF current. The RF voltage system may be split in two: a couple of voltage dividers and a processing circuit for the potential difference determination. Applying the RF current and voltage signals to the multiplier circuit it is possible to determine the RF power fed to the plasma. In this work a total of ten Rogowski coils, with 18mV/A sensibility constant, as well as twelve voltage dividers, capable of reducing a 10kV signal to approximately 5V signal, six voltage processing circuits and four signal multipliers, were built. Besides that, one demodulator circuit, capable of processing, simultaneously, the signals from four magnetic coils, was built too. All the devices constructed in this project were designed to be able to process signals with frequencies in the range of 3 to 6M Hz and produce a low frequency result signal that may be acquired automatically by the TCABR data acquisition system called TCAqs. For the calibration procedures and operational tests of the equipments developed in this work, it was established an Automated Calibration System (SCA) with a software application as one of its components that is capable of communicating and controlling test instruments, like oscilloscopes and function generators, through the communication port RS-232 and SCPI language. This software, called SCO, was fully developed using free and open source software in order to be used in Unix-Like operational systems like GNU/Linux. As a free software SCO was registered under the GNU/GPL license. The calibration procedures once operating with this system, whose principal characteristics is its automation functionality, allowed us to acquire a great quantity of data, that would have not been possible or practical to do manually. As a consequence, the resulting calibration curves may be considered more accurate, from an statistical point of view which enhanced considerably the quality of the results. After the characterization and detailed tests of all these devices off the TCABR and after the installation of the diagnostics in the TCABR, we may finally conclude they are ready to be used in experimental campaign.
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Gonçalves, Diego Antonio Falceta. ""Plasmas empoeirados: ventos estelares e o meio interestelar"". Universidade de São Paulo, 2005. http://www.teses.usp.br/teses/disponiveis/14/14131/tde-10082006-193654/.
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Neste trabalho primeiramente estudamos os efeitos na propagação de ondas de Alfvén em plasmas empoeirados encontrados em inúmeros ambientes astrofísicos. A relação de dispersão da onda é modificada apresentando novos mecanismos de amortecimento. Há na literatura dados observacionais que indicam a existência de condições para crescimento de partículas de poeira na base da atmosfera de estrelas gigantes e supergigantes frias. Construímos um modelo de perda de massa para essas estrelas no qual mostramos que um fluxo de ondas de Alfvén, amortecido pela presença de poeira, pode contribuir para a geração de um vento de baixa velocidade e alta taxa de perda de massa, de acordo com as observações. Já no caso de estrelas quentes, mostramos como é possível obter as condições ideais para formação e crescimento destas partículas em um modelo de colisão de ventos em sistemas binários. A partir deste modelo, é possível explicar as altas emissões em raios-X observadas, além do crescimento de grãos no pós-choque. Aplicando a idéia ao sistema binário de eta Carinae, o modelo permite a determinação dos parâmetros orbitais do sistema. A poeira contida nos ventos estelares é então ejetada para o meio interestelar. Através de um cálculo semi-empírico determinamos a importância de cada intervalo de massa estelar, em cada etapa evolutiva, no retorno de material sólido ao MI. Em regiões de formação estelar investigamos como as ondas de Alfvén, amortecidas pela presença de poeira, influenciam a estabilidade de nuvens moleculares. Em oposição às teorias encontradas na literatura, mostramos que uma nuvem molecular anã, suportada apenas por pressão magnética, não pode ser dinamicamente estável.In this work, we firstly discuss the propagation of Alfvén waves in dusty plasmas found in several astrophysical environments. The wave dispersion relation is modified giving rise to new damping mechanisms. There are in the literature observational data indicating the presence of dust near the surface of cool giant and supergiant stars. We developed a stellar mass loss model where we show that a flux of Alfvén waves, damped by the dust presence,can generate a low velocity and high mass loss rate wind, in agreement with the observations. In the case of hot stars we show how it is possible to obtain the special conditions for dust growth in a wind collision model of massive binary systems. For this model it is possible to explain both, the high X-rays emissions and dust growth at the post-shock phase. Applying the idea to the $eta$ Carinae binary system, the model allows the determination of the system orbital and the stellar wind parameters. The stellar wind´s dust is then ejected to the interstellar medium. In a semi-empirical calculation we showed the importance of each stellar mass, at each evolutionary phase, on the dust feedback of the ISM. For star formation regions, we investigate the role of Alfvén waves, damped by the dust presence, on the stability of the molecular clouds. In spite of the works found in the literature, we showed that a dwarf molecular cloud, magnetically supported only, is unstable.
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Puglia, Paulo Giovane Paschoali Pereira. "Identificação e localização de ondas de Alfvén excitadas no plasma de um tokamak". Universidade de São Paulo, 2015. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-24092015-141928/.
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O objetivo deste trabalho é a investigação da excitação e detecção de ondas globais de Alfvén no plasma do tokamak TCABR para fins diagnósticos. As ondas são excitadas com o uso de uma ou duas antenas localizadas dentro do vaso do TCABR. Para excitar o modo global de Alfvén, as antenas são alimentadas com corrente de radio-frequência de até $15$A cada, na faixa de frequência de $2-4 MHz$. O esquema apresentado nos permitiu estimar o valor da massa efetiva no centro do plasma, que tem seu valor afetado pela concentração de impurezas. O amplificador de corrente para as antenas é baseado no chaveamento de MOSFETs. As ondas são excitadas com o uso de baixa potência, assim não causam perturbação nos parâmetros básicos do plasma. Foi verificada a variação da frequência de ressonância do modo global de Alfvén com a densidade do plasma. A localização da ressonância do modo é identificada na parte central do plasma, devido ao batimento da amplitude da onda com oscilações dente de serra, de modo que a inversão de fase entre o batimento e a oscilação dente de serra melhora a precisão da determinação da condição ressonante. A paridade toroidal dos modos excitados é determinada com o uso de duas antenas localizadas em posição toroidal oposta na câmara do TCABR e com diferença de fase na corrente de radio-frequência. O conhecimento do número de onda toroidal é importante para a correta estimativa da localização do modo excitado e do valor da massa efetiva do plasma. O valor obtido para a estimativa da massa efetiva, primeiramente, foi mais alto que nossa expectativas e não era bem relacionado com estimativas da condutividade do plasma. O valor obtido foi de $A_{eff}\\approx 1.60$, com um erro sistemático. Para calibrar a densidade central do plasma usamos dados do reflectômetro e realizamos disparos com gás hélio, que tem a mesma massa efetiva que a maioria das impurezas do TCABR. Finalmente, estimamos a massa efetiva como $A_{eff} = 1.40 \\pm 0.07$, valor compatível com a estimativa de $Z_{eff}$.The goal of this study is experimental detection of global Alfvén waves in the plasma of TCABR tokamak for diagnostic. The waves are excited by the use of one or two antennas posed within the shadow of the limiter within the TCABR vessel. To excite the global Alfvén eigenmode the antennas are fed with radio-frequency current of up to $ 15$A each, in the frequency range of $ 2-4 $ MHz. The presented scheme allows us to estimate the value of the effective mass in the centre of the plasma, which has its value affected by the concentration of impurities in the plasma. The amplifier of the antenna current is based on electronically switching MOSFETs. The waves are excited in the plasma with low power, thus it does not cause perturbation of the basic plasma parameters. The variation of the resonance frequency of the global Alfvén eigenmode with density is verified. The location of the resonance is identified in the central part of the plasma due to the wave amplitude beating with sawtooth oscillations, so that the phase inversion between the beating and the sawtooth oscillation improves the accuracy of determining the resonant condition. The toroidal parity of the excited modes is determined with use of two antennas oppositely located within the TCABR chamber and established by phase difference between their radio-frequency current. Knowledge of the toroidal wave number is important for a correct estimate of both the excited mode location and the plasma effective ion mass value. The value of the initially found effective mass was $ A_ {eff} \\approx 1.60$, higher than our expectations at first and did not agree with plasma conductivity estimates, and we proposed that it had a systematic error of approximately $10\\%$. To calibrate the central plasma density, it was used data from a reflectometer and some plasma discharges performed with helium gas, which has the same effective mass as most TCABR impurities. Finally, we estimate the effective mass as $ A_ {eff} = 1.40 \\pm 0.07$, that is consistent with the $ Z_ {eff} $ estimation.
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Souza, Fábio Camilo de. "Teoria de ondas em Tokamaks". Universidade de São Paulo, 2016. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-20092016-141959/.
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Esta dissertação se propõe a uma investigação teórica sobre a propagação de ondas de Alfvén e geodésicas no plasma de um Tokamak, destacando suas funcionalidades na viabilidade da construção de um futuro reator de fusão nuclear para a produção de energia. O Tokamak se trata de uma câmara toroidal onde o plasma fica confinado sob efeitos de um forte campo magnético a fim de alcançar altas temperaturas, necessárias para atingir as condições necessárias para a fusão nuclear. Foram abordadas as ondas de Alfvén e mais profundamente os Modo Acústico Geodésicos. Para ondas de Alfvén estão descritas, a sua natureza, uma onda comum a qualquer plasma sujeito a um campo magnético, quando devidamente perturbado ondas de Alfvén se propagam ao longo destas linhas de campo, também são relatadas suas possíveis aplicações. É descrito um estudo teórico onde se encontra os modos de Alfvén em coordenadas cilíndricas, uma aproximação para tokamaks com alta razão de aspecto. No caso dos Modos Acústico Geodésicos, GAM, onde sua origem está na curvatura toroidal do Tokamak, se tratam de perturbação de pressão que se propaga poloidalmente, tendo configurações simétricas ao longo do toroide, possuindo número toroidal $N=0$, e número poloidal $M=0,\\pm 1,\\pm 2 , ... $. É abordado suas possíveis aplicações e também um efeito de natureza estranha onde modos de Alfvén interagem com GAM. Por fim, segue uma investigação teórica sobre os efeitos de rotação de elétrons e íons, na forma do fluxo de cada partícula ao longo das linhas de campo magnético, na relação de dispersão e instabilidades de GAM. Em prosseguimento à investigação teórica sobre os efeitos de rotação, segue uma breve análise de dados fornecidos pelo Instituto de Física de Plasma da Academia Tcheca de Ciências, obtidos no COMPASS, onde é demonstrada uma possível correspondência qualitativa da dispersão e instabilidades de GAM com a teoria desenvolvida.This work intends to present a theorical treatment of Alfven and geodesic wave behavior in tokamak plasma, showing their function on the viability study for the construction of a fusion reactor for energy production. The Tokamak is a toroidal chamber where the plasma stays confined under effects of a strong magnetic field where its can reach high temperature in necessary conditions for nuclear fusion. It is presented the behavior of Alfvén waves and deeper Geodesic Acoustic Modes. For Alfvén waves, it is described it\'s nature, a comum wave in any plasma under magnetic field, when properly perturbed, Alfvén waves can propagate on the magnetic field line, also it is presented possible applications. It\'s presented a theorical treatment where Alfvén modes in cilindrical coordinates, approximation for Tokamak with high aspect ratio. In Geodesic Acoustic Mode, GAM, driven by the todoidal curvature and symmetry of Tokamak, it is showed possible applications and a interaction with Alfvén waves. A perturbation that propagate in poloidal direction, symmetrical in toroidal direction, with toroidal number $N=0$ and poloidal number $M = 0, \\pm 1, \\pm 2 , ...$, a theorical treatment on rotation effects of electrons and ions in form of flux along the magnetic field line, on dispersion relation and instability of GAM is presented. In the end, it is presented a data analysis on COMPASS shoots, where is showed a possible qualitative correspondence between GAM dispersion and instabilities with the theory and experiment.
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Chang, Ouliang. "Numerical Simulation of Ion-Cyclotron Turbulence Generated by Artificial Plasma Cloud Release". Thesis, Virginia Tech, 2009. http://hdl.handle.net/10919/34018.
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Possibilities of generating plasma turbulence to provide control of space weather processes have been of particular interest in recent years. Such turbulence can be created by chemical released into a magnetized background plasma. The released plasma clouds are heavy ions which have ring velocity distribution and large free energy to drive the turbulence. An electromagnetic hybrid (fluid electrons and particle ions) model incorporating electron inertia is developed to study the generation and nonlinear evolution of this turbulence. Fourier pseudo-spectral methods are combined with finite difference methods to solve the electron momentum equations. Time integration is accomplished by a 4th-order Runge-Kutta scheme or predicator-corrector method. The numerical results show good agreement with theoretical prediction as well as provide further insights on the nonlinear turbulence evolution. Initially the turbulence lies near harmonics of the ring plasma ion cyclotron frequency and propagates nearly perpendicular to the background magnetic field as predicted by the linear theory. If the amplitude of the turbulence is sufficiently large, the quasi-electrostatic short wavelength ion cyclotron waves evolve nonlinearly into electromagnetic obliquely propagating shear Alfven waves with much longer wavelength. The results indicate that ring densities above a few percent of the background plasma density may produce wave amplitudes large enough for such an evolution to occur. The extraction of energy from the ring plasma may be in the range of 10-15% with a generally slight decrease in the magnitude as the ring density is increased from a few percent to several 10's of percent of the background plasma density. Possibilities to model the effects of nonlinear processes on energy extraction by introducing electron anomalous resistivity are also addressed. Suitability of the nonlinearly generated shear Alfven waves for applications to scattering radiation belt particles is discussed.Master of Science
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Sakaue, Takahito. "Nonlinear Alfvén Wave Model for Solar/Stellar Chromosphere, Corona and Wind from the Sun to M Dwarfs". Doctoral thesis, Kyoto University, 2021. http://hdl.handle.net/2433/263472.
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Tholerus, Emmi. "The dynamics of Alfvén eigenmodes excited by energetic ions in toroidal plasmas". Licentiate thesis, KTH, Fusionsplasmafysik, 2015. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-163127.
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Experiments for the development of fusion power that are based on magnetic confinement deal with plasmas that inevitably contain energetic (non-thermal) particles. These particles come e.g. from fusion reactions or from external heating of the plasma. Ensembles of energetic ions can excite plasma waves in the Alfvén frequency range to such an extent that the resulting wave fields redistribute the energetic ions, and potentially eject them from the plasma. The redistribution of ions may cause a substantial reduction heating efficiency, and it may damage the inner walls and other components of the vessel. Understanding the dynamics of such instabilities is necessary to optimise the operation of fusion experiments and of future fusion power plants. A Monte Carlo model that describes the nonlinear wave-particle dynamics in a toroidal plasma has been developed to study the excitation of the abovementioned instabilities. A decorrelation of the wave-particle phase is added in order to model stochasticity of the system (e.g. due to collisions between particles). Based on the nonlinear description with added phase decorrelation, a quasilinear version of the model has been developed, where the phase decorrelation has been replaced by a quasilinear diffusion coefficient in particle energy. When the characteristic time scale for macroscopic phase decorrelation becomes similar to or shorter than the time scales of nonlinear wave-particle dynamics, the two descriptions quantitatively agree on a macroscopic level. The quasilinear model is typically less computationally demanding than the nonlinear model, since it has a lower dimensionality of phase space. In the presented studies, several effects on the macroscopic wave-particle dynamics by the presence of phase decorrelation have been theoretically and numerically analysed, e.g. effects on the growth and saturation of the wave amplitude, and on the so called frequency chirping events with associated hole-clump pair formation in particle phase space. Several effects coming from structures of the energy distribution of particles around the wave-particle resonance has also been studied.QC 20150330
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Tholerus, Emmi. "The dynamics of Alfvén eigenmodes excited by energetic ions in toroidal plasmas". Doctoral thesis, KTH, Fusionsplasmafysik, 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-193029.
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The future fusion power plants that are based on magnetic confinement will deal with plasmas that inevitably contain energetic (non-thermal) particles. These particles come, for instance, from fusion reactions or from external heating of the plasma. Ensembles of energetic ions can excite eigenmodes in the Alfvén frequency range to such an extent that the resulting wave fields redistribute the energetic ions, and potentially eject them from the plasma. The redistribution of ions may cause a substantial reduction of heating efficiency. Understanding the dynamics of such instabilities is necessary to optimise the operation of fusion experiments and of future fusion power plants. Two models have been developed to simulate the interaction between energetic ions and Alfvén eigenmodes. One is a bump-on-tail model, of which two versions have been developed: one fully nonlinear and one quasilinear. The quasilinear version has a lower dimensionality of particle phase space than the nonlinear one. Unlike previous similar studies, the bump-on-tail model contains a decorrelation of the wave-particle phase in order to model stochasticity of the system. When the characteristic time scale for macroscopic phase decorrelation is similar to or shorter than the time scale of nonlinear wave-particle dynamics, the nonlinear and the quasilinear descriptions quantitatively agree. A finite phase decorrelation changes the growth rate and the saturation amplitude of the wave mode in systems with an inverted energy distribution around the wave-particle resonance. Analytical expressions for the correction of the growth rate and the saturation amplitude have been derived, which agree well with numerical simulations. A relatively weak phase decorrelation also diminishes frequency chirping events of the eigenmode. The second model is called FOXTAIL, and it has a wider regime of validity than the bump-on-tail model. FOXTAIL is able to simulate systems with multiple eigenmodes, and it includes effects of different individual particle orbits relative to the wave fields. Simulations with FOXTAIL and the nonlinear bump-on-tail model have been compared in order to determine the regimes of validity of the bump-on-tail model quantitatively. Studies of two-mode scenarios confirmed the expected consequences of a fulfillment of the Chirikov criterion for resonance overlap. The influence of ICRH on the eigenmode-energetic ion system has also been studied, showing qualitatively similar effects as seen by the presence of phase decorrelation. Another model, describing the efficiency of fast wave current drive, has been developed in order to study the influence of passive components close to the antenna, in which currents can be induced by the antenna generated wave field. It was found that the directivity of the launched wave, averaged over model parameters, was lowered by the presence of passive components in general, except for low values of the single pass damping of the wave, where the directivity was slightly increased, but reversed in the toroidal direction.De framtida fusionskraftverken baserade på magnetisk inneslutning kommer att hantera plasmor som oundvikligen innehåller energetiska (icke-termiska) partiklar. Dessa partiklar kommer exempelvis från fusionsreaktioner eller från externa uppvärmningsmekanismer av plasmat. Ensembler av energetiska joner kan excitera egenmoder i Alfvén-frekvensområdet i en sådan utsträckning att de resulterande vågfälten omfördelar de energetiska jonerna i rummet, och potentiellt slungar ut jonerna ur plasmat. Omfördelningen av joner kan orsaka en väsentligen minskad uppvärmningseffekt. Det är nödvändigt att förstå dynamiken hos denna typ av instabilitet för att kunna optimera verkningsgraden hos experiment och hos framtida fusionskraftverk. Två modeller har utvecklats för att simulera interaktionen mellan energetiska joner och Alfvén-egenmoder. Den första är en bump-on-tail-modell, av vilken två versioner har utvecklats: en fullt icke-linjär och en kvasi-linjär. I den kvasi-linjära versionen har partiklarnas fasrum en lägre dimensionalitet än i den icke-linjära versionen. Till skillnad från tidigare liknande studier innehåller denna bump-on-tail-modell en dekorrelation av våg-partikelfasen för att modellera stokasticitet hos systemet. När den karakteristiska tidsskalan för makroskopisk fasdekorrelation är ungefär samma som eller kortare än tidsskalan för icke-linjär våg-partikeldynamik så stämmer den icke-linjära och den kvasi-linjära beskrivningen överens kvantitativt. En ändlig fasdekorrelation förändrar vågmodens tillväxthastighet och satureringsamplitud i system med en inverterad energifördelning omkring våg-partikelresonansen. Analytiska uttryck för korrektionen av tillväxthastigheten och satureringsamplituden har härletts, vilka stämmer väl överens med numeriska simuleringar. En relativt svag fasdekorrelation försvagar även "frequency chirping events" (snabba frekvensskiftningar i korttids-Fourier-transformen av egenmodens amplitudutveckling) hos egenmoden. Den andra modellen, kallad FOXTAIL, har ett mycket bredare giltighetsområde än bump-on-tail-modellen. FOXTAIL kan simulera system med flera egenmoder, och den inkluderar effekter av olika enskilda partikelbanor relativt vågfälten. Simuleringar med FOXTAIL och med bump-on-tail-modellen har jämförts för att kvantitativt bestämma bump-on-tail-modellens giltighetsområde. Studier av scenarier med två egenmoder bekräftar de förväntade effekterna av när Chirikov-kriteriet för resonansöverlapp uppfylls. Även inflytandet av ICRH på dynamiken mellan egenmoder och energetiska joner har studerats, vilket har visat kvalitativt liknande effekter som har observerats i närvaron av fasdekorrelation. En annan modell, vilken beskriver effektiviteten hos "fast wave current drive" (strömdrivning med snabba magnetosoniska vågor), har utvecklats för att studera inflytandet av passiva komponenter nära antennen, i vilka strömmar kan induceras av vågfälten som genereras av antennen. Det visades att den utskickade vågens direktivitet, medelvärdesbildat över modellparametrar, generellt sett minskade vid närvaron av passiva komponenter, förutom vid låg "sinlge pass damping" (dämpning av vågen vid propagering genom hela plasmat), då direktiviteten istället ökade något, men bytte tecken i toroidal riktning.
QC 20160927
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Lee, Bo Ram Verfasser], Dieter [Akademischer Betreuer] [Hoffmann i Christoph [Akademischer Betreuer] Niemann. "Study of a laser generated diamagnetic cavity and Alfvén waves in a large magnetized plasma / Bo Ram Lee. Betreuer: Dieter H. H. Hoffmann ; Christoph Niemann". Darmstadt : Universitäts- und Landesbibliothek Darmstadt, 2015. http://d-nb.info/1112044752/34.
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Lee, Bo Ram [Verfasser], Dieter [Akademischer Betreuer] Hoffmann i Christoph [Akademischer Betreuer] Niemann. "Study of a laser generated diamagnetic cavity and Alfvén waves in a large magnetized plasma / Bo Ram Lee. Betreuer: Dieter H. H. Hoffmann ; Christoph Niemann". Darmstadt : Universitäts- und Landesbibliothek Darmstadt, 2015. http://nbn-resolving.de/urn:nbn:de:tuda-tuprints-52112.
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Schreiner, Anne [Verfasser], i Joachim [Gutachter] Saur. "A Model for Dissipation of Solar Wind Turbulence with Damping by Kinetic Alfvén Waves: Comparison with Observations and Implications for the Dissipation Process in the Solar Wind / Anne Schreiner ; Gutachter: Joachim Saur". Köln : Universitäts- und Stadtbibliothek Köln, 2017. http://d-nb.info/113762423X/34.
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Eilers, Bischoff Jens, i Sebastian Jovancic. "Variability of Io’s Aurora and the Moon’s Footprint on Jupiter". Thesis, KTH, Skolan för elektroteknik och datavetenskap (EECS), 2020. http://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-293888.
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We study the variability of intensity of Io’s aurora asa function of Jupiter’s rotation measured in system III longitude.The far-ultraviolet intensity of Io’s aurora was measured by theHubble Space Telescope (HST) using the FUV-MAMA photondetector of the STIS. The data was processed using Matlab tofilter background and reflection, and account for the detector’soptical systems. Target regions of the detector were isolated forthe measurement of the OI(1356 ̊A) and SI(1479 ̊A) emissionsrespectively. By sampling photon detections within each emissionregion, we compute intensity reconstructions that we map tosystem III longitude. Curves were then fitted to the reconstruc-tions using a sinus fit. The results show two intensity peaks atsystem III longitudes (140±5)◦and (284±2)◦for both OIandSI. The difference in amplitude between the peaks are (38±6)%and (28±6)% for OIand SIrespectively. The asymmetriespeak intensities is possibly caused by the probability of excitingsulphur being higher than the probability of exciting sulphur.For a full explanation measurement of the oxygen to sulphurproportion in Ios atmosphere would be needed. We compare theresults to peaks of Io’s footprint on Jupiter measured by JUNOand other HST data sets. We find it likely that we confirm furthervariance in peak angle than reported in other research. This isespecially clear in the first intensity peak as it has a significantlylarger angle. Variability in Jupiter’s magnetic field and densityof the Jovian plasma torus is likely to explain peak angle andintensity variability, but further research is necessary to explainthe mechanisms in detail.Vi studerar hur intensiteten av Ios aurora varierar i relation till Jupiters rotation mätt i system III longitud. Ios aurora mättes inom UVC området av Hubble Space Telescope (HST) med FUV-MAMA fotondetektorn. Matlab användes för att filtrera bort oönskade signaler som reflektion och bakgrund samt ta hänsyn till sensorns optiska system. Observationsområderna på sensorn konstruerades för mätningen av syre OI (1356Å ) och svavel SI (1479Å ) emissionerna. Genom att sampla fo- tondetektioner inom varje observationsområde så rekonstruerar vi en intensitetskurva som vi mappar till system III longitud. En kurva var sedan anpassad till rekonstruktionen med hjälp av en sinusanpassning. Resultaten visar två intensitetstoppar vid system III longituderna (140 ± 5)◦ och (284 ± 2)◦ för både OI och SI . Kvoten mellan topparna var (38 ± 6)% för OI och (28 ± 6)% för SI . Skillnaden i topparna kan förklaras av att sannolikheten att excitera svavel är större än att excitera syre. För fullständig beskrivning av skillnaden i topparna skulle mätningar av syre till svavel proportionen i Ios atmosfär behövas. Vi jämför våra reslutat med mätningar av Ios avtryck på Jupiter från JUNO och andra HST mätningar. Vi finner det sannolikt att vi bekräftar ytterligare varians i topparnas vinkel, främst för den första toppen vars vinkel är signifikant större. Variationer i Jupiters magnetfält och plasmadensitet av Jupiters plasmatorid kan sannolikt förklara positionen av topparna och intensitetsvariationerna. Vidare forskning behövs för att utförligt förklara dessa mekanismer.
Kandidatexjobb i elektroteknik 2020, KTH, Stockholm
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Vedin, Jörgen. "Numerical modeling of auroral processes". Doctoral thesis, Umeå University, Physics, 2007. http://urn.kb.se/resolve?urn=urn:nbn:se:umu:diva-1117.
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One of the most conspicuous problems in space physics for the last decades has been to theoretically describe how the large parallel electric fields on auroral field lines can be generated. There is strong observational evidence of such electric fields, and stationary theory supports the need for electric fields accelerating electrons to the ionosphere where they generate auroras. However, dynamic models have not been able to reproduce these electric fields. This thesis sheds some light on this incompatibility and shows that the missing ingredient in previous dynamic models is a correct description of the electron temperature. As the electrons accelerate towards the ionosphere, their velocity along the magnetic field line will increase. In the converging magnetic field lines, the mirror force will convert much of the parallel velocity into perpendicular velocity. The result of the acceleration and mirroring will be a velocity distribution with a significantly higher temperature in the auroral acceleration region than above. The enhanced temperature corresponds to strong electron pressure gradients that balance the parallel electric fields. Thus, in regions with electron acceleration along converging magnetic field lines, the electron temperature increase is a fundamental process and must be included in any model that aims to describe the build up of parallel electric fields. The development of such a model has been hampered by the difficulty to describe the temperature variation. This thesis shows that a local equation of state cannot be used, but the electron temperature variations must be descibed as a nonlocal response to the state of the auroral flux tube. The nonlocal response can be accomplished by the particle-fluid model presented in this thesis. This new dynamic model is a combination of a fluid model and a Particle-In-Cell (PIC) model and results in large parallel electric fields consistent with in-situ observations.
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Blanco-Benavides, Jose Mauricio. "Electron acceleration by Inertial Alfven Waves". Master's thesis, 2011. http://hdl.handle.net/10048/1786.
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The nightside auroral region is known to be the most powerful source of radiation from Earth to space. Emitted radiation reaches up to 10^9 watt, with frequencies ranging 100 - 600 kHz, and is known as Auroral Kilometric radiation (AKR).
AKR is generated through coherent emission by highly energetic electrons. In order to understand how these electrons are energized, a 1D test particle code has been written to study wave-particle interactions at the inertial regime. The computational model reproduces particle dynamics and wave properties in uniform and non-uniform conditions of magnetic field and plasma density. Simulations of wave-particle interactions have also been performed and resulting observations were compared with similar publications. The model is intended to be used to obtain unstable particle distributions that are characteristic of the auroral region, and will be utilized in future studies of generation mechanisms of AKR.
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Kortbawi, David. "Alfven wave studies on a tokamak". 1987. http://catalog.hathitrust.org/api/volumes/oclc/17852866.html.
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Hirsch, Michael. "Alfvén waves underlying ionospheric destabilization: ground-based observations". Thesis, 2017. https://hdl.handle.net/2144/23382.
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During geomagnetic storms, terawatts of power in the million mile-per-hour solar wind pierce the Earth’s magnetosphere. Geomagnetic storms and substorms create transverse magnetic waves known as Alfvén waves. In the auroral acceleration region, Alfvén waves accelerate electrons up to one-tenth the speed of light via wave-particle interactions. These inertial Alfvén wave (IAW) accelerated electrons are imbued with sub-100 meter structure perpendicular to geomagnetic field B. The IAW electric field parallel to B accelerates electrons up to about 10 keV along B. The IAW dispersion relation quantifies the precipitating electron striation observed with high-speed cameras as spatiotemporally dynamic fine structured aurora.
A network of tightly synchronized tomographic auroral observatories using model based iterative reconstruction (MBIR) techniques were developed in this dissertation. The TRANSCAR electron penetration model creates a basis set of monoenergetic electron beam eigenprofiles of auroral volume emission rate for the given location and ionospheric conditions. Each eigenprofile consists of nearly 200 broadband line spectra modulated by atmospheric attenuation, bandstop filter and imager quantum efficiency. The L-BFGS-B minimization routine combined with sub-pixel registered electron multiplying CCD video stream at order 10 ms cadence yields estimates of electron differential number flux at the top of the ionosphere.
Our automatic data curation algorithm reduces one terabyte/camera/day into accurate MBIR-processed estimates of IAW-driven electron precipitation microstructure. This computer vision structured auroral discrimination algorithm was developed using a multiscale dual-camera system observing a 175 km and 14 km swath of sky simultaneously. This collective behavior algorithm exploits the “swarm” behavior of aurora, detectable even as video SNR approaches zero. A modified version of the algorithm is applied to topside ionospheric radar at Mars and broadcast FM passive radar. The fusion of data from coherent radar backscatter and optical data at order 10 ms cadence confirms and further quantifies the relation of strong Langmuir turbulence and streaming plasma upflows in the ionosphere with the finest spatiotemporal auroral dynamics associated with IAW acceleration. The software programs developed in this dissertation solve the century-old problem of automatically discriminating finely structured aurora from other forms and pushes the observational wave-particle science frontiers forward.
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Ghanesh, N. "MHD Waves Driven by Small-scale Motion and Implications for the Earth's Core". Thesis, 2017. http://etd.iisc.ernet.in/2005/3580.
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Rotating convection in the Earth's core produces columnar vortices of radius ~10 km or less near the inner core boundary. Small-scale motions in the core can travel as Alfvén waves in the face of Ohmic diffusion, provided the ratio of the magnetic diffusion time th to the Alfvén wave travel time tA (measured by the Lundquist number S0) is much greater than unity. These motions transfer angular momentum from the core to the mantle, a process that can help explain variations in length of day. Vortices subject to the combined influence of a magnetic field and background rotation give rise to fast and slow Magneto-Coriolis (MC) waves whose damping is not well understood. This thesis investigates the long-time evolution of magneto hydrodynamic (MHD) waves generated by an isolated, small-scale motion in an otherwise quiescent, electrically conducting fluid. The first part of the study focuses on the damping of small-scale Alfvén waves, which is independent of rotation. For a plausible magnetic field strength in the Earth's core, it is shown that flows of lengthscale ~ 5 km or larger can propagate across the core as damped Alfvén waves on sub-decadal timescales. The second part of the study looks at MC waves generated from an isolated blob under rotation and a uniform axial magnetic field. The decay laws for these waves are obtained by considering the decay of fast and slow waves individually. While the fast waves are subject to strongly anisotropic magnetic diffusion, the slow waves diffuse isotopically. New timescales are derived for the onset of damping and the transition from the wave-dominated to the diffusion-dominated (quasi-static) phase of decay. This study shows for the first time that MC waves originating from small-scale vortices of magnetic Reynolds number Rm ~ 1 can be long-lived. The results of this study are extendible to small-scale MHD turbulence under rotation, whose damped wave phase has not been adequately addressed in the literature. Furthermore, it is thought that this study would help place a lower bound on the poloidal magnetic field strength in the Earth’s core.
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Thuecks, Derek Jon Kletzing Craig A. "Laboratory investigations of dispersive Alfvén waves and their role in electron acceleration". 2009. http://ir.uiowa.edu/etd/268/.
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Sedeh, Leila Norouzi. "Doppler clutter in HF radar systems produced by ULF waves". Thesis, 2014. http://hdl.handle.net/1959.13/1042283.
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Research Doctorate - Doctor of Philosophy (PhD)Ultra low frequency (ULF) waves are generated by the interaction of the solar wind with Earth’s magnetosphere. The waves propagate through the ionosphere and may be seen in data from SuperDARN Over-The-Horizon radars as oscillations in Doppler velocity which coincide with oscillations of the geomagnetic field recorded by ground magnetometers. Data from the two Tasman International Geospace Environment Radars (TIGER) and the magnetometer located on Macquarie Island over 2006-2009 show that ULF wave signatures are common. The dependence with time of day showed most ULF radar events occurred between 6-12 UT (dusk and pre-mid-night sector). Using the Maximum Entropy Method (MEM) several spectral aspects of detected ULF waves were investigated for the first time. Most of the recorded frequencies were in the range 1- 4 mHz. Some frequencies were seen more often than others with the more common frequencies spaced about 0.3mHz apart, consistent with previous studies. There was no evidence of a frequency dependence on latitude. Field line resonance (FLR) signatures in the radar data were expected but were not common, as shown by comparisons with coincident ground magnetometer data. This study has shown that most radar echoes containing ULF wave Doppler signatures appear to be backscattered from the plasmapause region mapped into the ionosphere. Modelling of the Doppler velocity combined with a ULF wave model and two dimensional ray tracing was achieved for the first time. The results are consistent with experimental observations. With further improvement, this modelling should provide a valuable tool to understand shear Alfven mode and fast mode plasma wave interactions within the ionosphere and their effects on HF propagation through the ionosphere.
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Jaafari, Fajer Bitar. "Simulations of high-latitude ionosphere-magnetosphere region plasma density structures and the Alfven waves effects". 2009. http://hdl.handle.net/10106/1755.
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Chen, Ching-Chung, i 陳敬中. "A Simulation Study of Rotational Discontinuities and Nonlinear Alfven Waves in the Solar Wind". Thesis, 2006. http://ndltd.ncl.edu.tw/handle/534gks.
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碩士國立中央大學
太空科學研究所
94
This thesis work studies rotational discontinuities (RDs) by means of electron-ion two-fluid simulation and hybrid simulation (fluid electrons and kinetic ions). We examine the evolution of RDs under different initial conditions. Our goal is to find the best initial conditions, which can yield the most stable RD structures. The results of this research show that, when the initial width of the RD transition region is less than 30 , short-wavelength and large-amplitude waves will be emitted from the transition region. As a result, the transition region widens gradually with time. The RD structure is relatively steady when the initial width of the RD is more than 90 , although it can still emit small-amplitude waves to both up-stream and down-stream sides. The width of the transition region keeps constant and becomes a stable hook-shaped rotational structure. Double-hook rotational structures and d-shaped rotational structures, which have never been obtained in the previous simulations, are found in this thesis study. The double-hook rotational structures obtained in this study are similar to the structures of RDs and Alfven waves observed in the solar wind.
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莊宏親. "He++ Acceleration by Alfven Waves in the Solar Wind: Formation of He++/H+ Differential Streams". Thesis, 1999. http://ndltd.ncl.edu.tw/handle/40010200007931549912.
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Wang, Ge active 2013. "Rapid frequency chirps of an Alfvén wave in a toroidal plasma". 2013. http://hdl.handle.net/2152/21380.
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Results from models that describe frequency chirps of toroidal Alfvén eigenmode excited by energetic particles are presented here. This structure forms in TAE gap and may or may not chirp into the continuum. Initial work described the particle wave interaction in terms of a generic Hamiltonian for the particle wave interaction, whose spatial dependence was xed in time. In addition, we have developed an improved adiabatic TAE model that takes into account the spatial prole variation of the mode and the nite orbit excursion from the resonant ux surfaces, for a wide range of toroidal mode numbers. We have shown for the generic xed prole model that the results from the adiabatic model agree very well with simulation result except when the adiabatic condition breaks down due to the rapid variations of the wave amplitude and chirping frequency. We have been able to solve the adiabatic problem in the case when the spatial prole is allowed to vary in time, in accord with the structure of the response functions, as a function of frequency. All the models predict that up-chirping holes do not penetrate into the continuum. On the other hand clump structures, which down chirp in frequency may, depending on detailed parameters, penetrate the continuum. The systematic theory is more restrictive than the generic theory, for the conditions that enable clump to penetrate into the continuum. In addition, the systematic theory predicts an important nite drift orbit width eect, which eventually limits and suppresses a down-chirping response in the lower continuum. This interruption of the chirping occurs when the trapped particles make a transition from intersecting both resonant points of the continuum to just one resonant point.text
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Chen-JiaWeng i 翁承嘉. "Effects of ion-neutral collisions on Alfvén waves and formation of compound discontinuity/shock structures". Thesis, 2013. http://ndltd.ncl.edu.tw/handle/gcyyvt.
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博士國立成功大學
物理學系碩博士班
101
Alfvén waves are low-frequency transverse waves propagating in a magnetized plasma. The presence of neutral particles may modify the wave frequency and cause damping of Alfvén waves. MHD discontinuity is a stationary thin layer through which the magnetic field, plasma density, pressure, and flow velocity may have a significant jump. In the first part of this thesis, we investigate the effect of ion-neutral collisions on the damping of Alfvén waves in a homogeneous plasma. In the second part of this thesis, 1-D Riemann problem is used to study the generation and evolution of MHD discontinuities associated with magnetic reconnection. First, the effects on Alfvén waves depend on two parameters: (1) , the ratio of neutral density and ion density , and (2) , the ratio of neutral collisional frequency by ions , , to the wave frequency . Most of previous studies examined only the limiting case with a relatively large neutral collisional frequency or . In the Chapter 2 of this thesis, the dispersion relation for Alfvén waves is solved for all values of and . It is found for the first time that there is a “forbidden zone” in the parameter space, where the real frequency of Alfvén waves becomes zero and Alfvén waves become evanescent. Approximate solutions in the limit as well as are obtained. We also discuss the propagation and damping of Alfvén waves in the ionosphere and in the solar chromosphere, where the “forbidden zone” is identified. Second, we use 1-D hybrid code to simulate the generation and evolution of MHD discontinuities associated with magnetic reconnection in a current sheet. As a result of the leakage of slow shock (SS), the ion parallel temperature and temperature anisotropy tends to increase, where is the ion parallel (perpendicular) beta. The propagation rotational discontinuity (RD) and slow shock (SS) lead to formation of various compound structures in the reconnection outflow region. Four types of compound structure are found in our simulations: (a) RD-SS compound structure: the RD is attached to the leading part of SS, (b) SS-RD (DD) compound structure: RD is attached to the rear part of SS, (c) SS-RD-SS compound structure: RD is trapped inside SS, and (d) switch-off slow shock (SSS) with a rotational wave train. The type of compound structure generated depends on the initial ion beta and magnetic shear angle .
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Lee, Bo Ram. "Study of a laser generated diamagnetic cavity and Alfvén waves in a large magnetized plasma". Phd thesis, 2015. https://tuprints.ulb.tu-darmstadt.de/5211/1/Diss_ver111_final.pdf.
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Dense plasma expansion into a tenuous magnetized background plasma is prevalent in space and astrophysical environments. In the interaction between plasmas with different densities under the influence of the magnetic field, various hydromagnetic waves are generated including the magnetized collisionless shocks which are believed to be the source of high energy particles, such as galactic cosmic rays from supernova remnants. Despite its importance in astrophysics and the study for longer than five decades, however, details of the shock physics, such as the formation process or the energy dissipation mechanisms are still not fully understood.
This work describes experiments carried out at the Large Plasma Device at University of California, Los Angeles, coupled to a kilojoule-laser. When a laser produced dense plasma interacts with a preformed, magnetized background plasma, a diamagnetic cavity is formed which can be pictured as a piston driving a collisionless shock. Understanding the micro-physics of generated diamagnetic cavities is crucial since it is observed in many magnetized plasmas with applied magnetic field and there are still a number of questions to be answered. In a series of experiments performed at different plasma parameters, magnetic flux probes and electron emissive probes are used to diagnose the structure of the diamagnetic cavity perpendicular to the magnetic field, especially at its edge where the collisionless coupling between the debris and ambient plasma takes place. In contrast to lower laser energy, a strong coupling to ambient ions could be observed depending on the background magnetic field although the energy conversion efficiency from the laser to the cavity stayed on the same order of magnitude. A rise of the radial electric field at the cavity edge was detected, which might be a direct evidence for the laminar coupling mechanism between debris and ambient plasmas without any collisional effects. Large fluctuations in the magnetic and electric field measurements in front of the cavity edge, which were also seen in the experimental observations, are assumed to be instabilities causing energy dissipation and the short cavity lifetime which is almost three orders of magnitude shorter than the theoretically derived classical diffusion time. Along the plasma column, soliton-like Alfv\'en waves were detected which might result from the nonlinear interaction between energetic electrons generated at the cavity edge and the surrounding magnetized plasma. Here, a better energy conversion efficiency from the laser to the Alfv\'en waves has been calculated. Finally, the experimental results are compared to two-dimensional hybrid simulations. The observed ion dynamics as well as large fluctuations in the electric field measurements at the cavity edge could be reproduced. An additional study was done on the effect of the polytropic coefficient in the electron temperature equation in the code and it showed that a nonadiabatic electron temperature increase affects the dynamics of the electric field as well as that of the diamagnetic cavity.