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Автор: Grafiati
Опубліковано: 6 вересня 2023

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Статті в журналах з теми "Alfevn Waves"

1

Rauf, S., and J. A. Tataronis. "Resonant four-wave mixing of finite-amplitude Alfvén waves." Journal of Plasma Physics 55, no. 2 (April 1996): 173–80. http://dx.doi.org/10.1017/s0022377800018766.

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Using the derivative nonlinear SchrÖdinger equation, resonant four-wave mixing of finite-amplitude Alfvén waves is explored in this paper. The evolution equations governing the amplitudes of the interacting waves and the conservation relations ale derived from the basic equation. These evolution equations are used to study parametric amplification and oscillation of two small-amplitude Alfvén waves due to two large-amplitude pump (Alfvén) waves. It is also shown that three pump waves can mix together to generate a low-frequency Alfven wave in a dissipative plasma.
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2

Kar, C., S. K. Majumdar, and A. N. Sekar Iyengar. "Stabilization of collisional drift waves by kinetic Alfvén waves." Journal of Plasma Physics 47, no. 2 (April 1992): 249–60. http://dx.doi.org/10.1017/s002237780002420x.

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We have investigated a mode-coupling mechanism between kinetic Alfvén waves and a collisional drift wave in an inhomogeneous cylindrical plasma. Drift waves satisfying the condition k⊥D > 1/r0 (where r0 is the radius of the plasma cylinder) are stabilized by the low-frequency ponderomotive force generated by the kinetic Alfvén waves. For typical plasma parameters and a moderate level of Alfven-wave intensity the stabilization factor is comparable to the destabilization mechanism due to collisions.
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3

Леонович, Анатолий, Anatoliy Leonovich, Цюган Цзун, Qiugang Zong, Даниил Козлов, Daniil Kozlov, Юнфу Ван, and Yongfu Wang. "Alfvén waves in the magnetosphere generated by shock wave / plasmapause interaction." Solar-Terrestrial Physics 5, no. 2 (June 28, 2019): 9–14. http://dx.doi.org/10.12737/stp-52201902.

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We study Alfvén waves generated in the magnetosphere during the passage of an interplanetary shock wave. After shock wave passage, the oscillations with typical Alfvén wave dispersion have been detected in spacecraft observations inside the magnetosphere. The most frequently observed oscillations are those with toroidal polarization; their spatial structure is described well by the field line resonance (FLR) theory. The oscillations with poloidal polarization are observed after shock wave passage as well. They cannot be generated by FLR and cannot result from instability of high-energy particle fluxes because no such fluxes were detected at that time. We discuss an alternative hypothesis suggesting that resonant Alfvén waves are excited by a secondary source: a highly localized pulse of fast magnetosonic waves, which is generated in the shock wave/plasmapause contact region. The spectrum of such a source contains oscillation harmonics capable of exciting both the toroidal and poloidal resonant Alfvén waves.
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4

Suzuki, T. K. "Coronal heating and wind acceleration by nonlinear Alfvén waves – global simulations with gravity, radiation, and conduction." Nonlinear Processes in Geophysics 15, no. 2 (March 26, 2008): 295–304. http://dx.doi.org/10.5194/npg-15-295-2008.

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Abstract. We review our recent results of global one-dimensional (1-D) MHD simulations for the acceleration of solar and stellar winds. We impose transverse photospheric motions corresponding to the granulations, which generate outgoing Alfvén waves. We treat the propagation and dissipation of the Alfvén waves and consequent heating from the photosphere by dynamical simulations in a self-consistent manner. Nonlinear dissipation of Alfven waves becomes quite effective owing to the stratification of the atmosphere (the outward decrease of the density). We show that the coronal heating and the solar wind acceleration in the open magnetic field regions are natural consequence of the footpoint fluctuations of the magnetic fields at the surface (photosphere). We find that the properties of the solar wind sensitively depend on the fluctuation amplitudes at the solar surface because of the nonlinearity of the Alfvén waves, and that the wind speed at 1 AU is mainly controlled by the field strength and geometry of flux tubes. Based on these results, we point out that both fast and slow solar winds can be explained by the dissipation of nonlinear Alfvén waves in a unified manner. We also discuss winds from red giant stars driven by Alfvén waves, focusing on different aspects from the solar wind.
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5

Mazur, V. A., and A. V. Stepanov. "Concerning the Dynamics of Energetic Protons in Coronal Magnetic Loops: Dispersion Effects of Alfven Waves." Symposium - International Astronomical Union 107 (1985): 559. http://dx.doi.org/10.1017/s0074180900076105.

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It is shown that the existence of plasma density inhomogeneities (ducts) elongated along the magnetic field in coronal loops, and of Alfven wave dispersion, associated with the taking into account of gyrotropy U ≡ ω/ωi ≪ 1 (Leonovich et al., 1983), leads to the possibility of a quasi-longitudinal k⊥ < √U k‖ propagation (wave guiding) of Alfven waves. Here ω is the frequency of Alfven waves, ωi is the proton gyrofrequency, and k is the wave number. It is found that with the parameter ξ = ω2 R/ωi A > 1, where R is the inhomogeneity scale of a loop across the magnetic field, and A is the Alfven wave velocity, refraction of Alfven waves does not lead, as contrasted to Wentzel's inference (1976), to the waves going out of the regime of quasi-longitudinal propagation. As the result, the amplification of Alfven waves in solar coronal loops can be important. A study is made of the cyclotron instability of Alfven waves under solar coronal conditions.
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6

Mazur, V. A., and A. V. Stepanov. "Concerning the Dynamics of Energetic Protons in Coronal Magnetic Loops: Dispersion Effects of Alfven Waves." Symposium - International Astronomical Union 107 (1985): 559. http://dx.doi.org/10.1017/s007418090007618x.

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It is shown that the existence of plasma density inhomogeneities (ducts) elongated along the magnetic field in coronal loops, and of Alfven wave dispersion, associated with the taking into account of gyrotropy U ≡ ω/ωi ≪ 1 (Leonovich et al., 1983), leads to the possibility of a quasi-longitudinal k⊥ < √U k‖ propagation (wave guiding) of Alfven waves. Here ω is the frequency of Alfven waves, ωi is the proton gyrofrequency, and k is the wave number. It is found that with the parameter ξ = ω2 R/ωi A > 1, where R is the inhomogeneity scale of a loop across the magnetic field, and A is the Alfven wave velocity, refraction of Alfven waves does not lead, as contrasted to Wentzel's inference (1976), to the waves going out of the regime of quasi-longitudinal propagation. As the result, the amplification of Alfven waves in solar coronal loops can be important. A study is made of the cyclotron instability of Alfven waves under solar coronal conditions.
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7

Nocera, Luigi, and Eric R. Priest. "Bistability of a forced hydromagnetic cavity." Journal of Plasma Physics 46, no. 1 (August 1991): 153–77. http://dx.doi.org/10.1017/s0022377800016007.

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We study the nonlinear stability of a one-dimensional hydromagnetic cavity into which Alfvén waves are fed by harmonic shear motions of its boundaries and where they interact with slow magnetosonic waves. We use characteristic conditions for the outgoing and ingoing Alfven waves at the boundaries where the magnetosonic oscillations are required to vanish. Forcing of Alfven waves takes place at a frequency close to the eigenfrequency of the lowest-order mode of the cavity. We let the frequency detuning δω vary as a free parameter together with the amplitude of the forcing, the plasma β and the compressive Reynolds number Re0. Given these last three parameters and varying δω, we calculate the amplitude of the nonlinear equilibrium state of the cavity as the stationary solution of a simple forced, dissipative dynamical system that governs the evolution of the cavity over a slow time scale and to which we are led by multiple-scale and Galerkin analyses of the one-dimensional MHD equations. This amplitude is a multi-valued function of δω (bistability), and we discuss the possibility of nonlinear stabilization of the Alfven wave by locking it in one of the bistable states. This amplitude undergoes saddle-node bifurcations: we calculate the two values of δω at which this occurs and the lowest value of the Reynolds number (27/2) for this to happen. We show that the magnetic energy density released during a bistable transition scales as (Re0)2; it has a maximum at β = 1 - (⅔)½ and it may amount to a substantial part of the energy originally stored in the unperturbed cavity. The magnetic power density released scales as (Re0)3 and has a maximum at β = 1 ± (⅓)½5. We conclude that the cavity is a good site for plasma heating such as that of the solar corona.
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8

Sallago, P. A. "LARGE AMPLITUDE ALFVÉN WAVES IN PARTIALLY IONIZED PLASMAS." Anales AFA 33, no. 3 (October 15, 2022): 85–89. http://dx.doi.org/10.31527/analesafa.2022.33.3.85.

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In this paper it is analyzed the propagation of large amplitude Alfvén waves in partially ionized plasmas (PIP) when electronic pressure, Hall and ambipolar terms of Ohm’s law are taken into account. Instead of linearizing and developing the perturbation in monochromatic waves, it is proposed that the perturbation satisfy the Alfvén wave’s conditions. As a result, a solution is found that in the fully ionized limit, it coincides with Sallago and Platzeck solution for Alfvénwaves in Hall magnetohydrodynamics (doi:10.1029/2003JA009920 ). Furthermore, if electronic pressure and Hall terms are null, in the linearized limit, the damping is equal to the one described by De Pontieu, B. Martens, P. C. H. and Hudson, H. S. (DOI = 10.1086/322408), if one imposes that the plasma is a perfect conductor.
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9

Леонович, Анатолий, Anatoliy Leonovich, Даниил Козлов, and Daniil Kozlov. "On ballooning instability in current sheets." Solnechno-Zemnaya Fizika 1, no. 2 (June 17, 2015): 49–69. http://dx.doi.org/10.12737/6425.

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The problem of instability of azimuthally small-scale Alfven and slow magnetosonic (SMS) waves in the geotail is solved. The solutions describe unstable oscillations in the presence of a current sheet and correspond to the region of stretched closed field lines of the magnetotail. The spectra of eigen-frequencies of several basic harmonics of standing Alfven and SMS waves are found in the local and WKB approximation, which are compared. It is shown that the oscillation properties obtained in these approximations differ radically. In the local approximation, the Alfven waves are stable in the entire range of magnetic shells. SMS waves go into the aperiodic instability regime (the regime of the ‘ballooning’ instability), on magnetic shells crossing the current sheet. In the WKB approximation, both the Alfven and SMS oscillations go into an unstable regime with a non-zero real part of their eigen-frequency, on magnetic shells crossing the current sheet. The structure of azimuthally small-scale Alfven waves across magnetic shells is determined.
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10

Guglielmi, Anatol, Boris Klain, and Alexander Potapov. "Alfvén waves: To the 80th anniversary of discovery." Solar-Terrestrial Physics 8, no. 2 (June 30, 2022): 69–70. http://dx.doi.org/10.12737/stp-82202210.

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The article is dedicated to the anniversary of the discovery of Alfvén waves. The concept of Alfvén waves has played an outstanding role in the formation and development of cosmic electrodynamics. A distinctive feature of Alfvén waves is that at each point in space the group velocity vector and the external magnetic field vector are collinear to each other. As a result, Alfvén waves can carry momentum, energy, and information over long distances. We briefly describe two Alfvén resonators, one of which is formed in the ionosphere, and the second presumably exists in Earth’s radiation belt. The existence of the ionospheric resonator is justified theoretically and confirmed by numerous observations. The second resonator is located between reflection points located high above Earth symmetrically with respect to the plane of the geomagnetic equator.
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Дисертації з теми "Alfevn Waves"

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.
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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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3

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).
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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.
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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.
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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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Анотація:
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
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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.
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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.
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Книги з теми "Alfevn Waves"

1

Cross, R. C. An introduction to Alfven waves. Bristol: Hilger, 1988.

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2

An introduction to Alfven waves. Bristol, England: A. Hilger, 1988.

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3

The physics of Alfvén waves. Berlin: Wiley-VCH, 2001.

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4

X, Zhang, and United States. National Aeronautics and Space Administration., eds. Magnetospheric filter effect for Pc 3 Alfven mode waves. [Huntsville, AL: University of Alabama in Huntsville, 1994.

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5

X, Zhang, and United States. National Aeronautics and Space Administration., eds. Magnetospheric filter effect for Pc 3 Alfven mode waves. [Huntsville, AL: University of Alabama in Huntsville, 1994.

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6

X, Zhang, and United States. National Aeronautics and Space Administration., eds. Magnetospheric filter effect for Pc 3 Alfven mode waves. [Huntsville, AL: University of Alabama in Huntsville, 1995.

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X, Zhang, and United States. National Aeronautics and Space Administration., eds. Magnetospheric filter effect for Pc 3 Alfven mode waves. [Huntsville, AL: University of Alabama in Huntsville, 1995.

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8

J, Rycroft Michael, ed. Whistler and Alfvén mode cyclotron masers in space. New York: Cambridge University Press, 2008.

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9

Bhattacharjee, A. Linear and non-linear studies of Alfven waves in space, grant period January 15, 1986 - January 14, 1990. [Washington, DC: National Aeronautics and Space Administration, 1990.

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10

Bhattacharjee, A. Linear and non-linear studies of Alfven waves in space, grant period January 15, 1986 - January 14, 1990. [Washington, DC: National Aeronautics and Space Administration, 1990.

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Частини книг з теми "Alfevn Waves"

1

Hollweg, Joseph V. "Alfvén Waves." In Mechanisms of Chromospheric and Coronal Heating, 423–34. Berlin, Heidelberg: Springer Berlin Heidelberg, 1991. http://dx.doi.org/10.1007/978-3-642-87455-0_72.

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2

Trakhtengerts, V. Yu. "The Turbulent Alfvén Layer." In Nonlinear Waves 3, 73–78. Berlin, Heidelberg: Springer Berlin Heidelberg, 1990. http://dx.doi.org/10.1007/978-3-642-75308-4_5.

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3

Goossens, M. "Alfvén Wave Heating." In Fragmented Energy Release in Sun and Stars, 51–62. Dordrecht: Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-1014-3_5.

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4

Golant, V. E., and V. I. Fedorov. "Alfvén Wave Heating." In RF Plasma Heating in Toroidal Fusion Devices, 169–77. Boston, MA: Springer US, 1989. http://dx.doi.org/10.1007/978-1-4684-1671-8_6.

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5

Boynton, G. Christopher, and ULF Torkelsson. "Nonlinear Dissipation of Alfvén Waves." In Magnetodynamic Phenomena in the Solar Atmosphere, 467–68. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0315-9_99.

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6

Tsurutani, Bruce T., Edward J. Smith, Christian M. Ho, Marcia Neugebauer, Bruce E. Goldstein, John S. Mok, Andre Balogh, David Southwood, and William C. Feldman. "Interplanetary Discontinuities and Alfvén Waves." In The High Latitude Heliosphere, 205–10. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0167-7_36.

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7

Goertz, C. K. "Discrete Breakup Arcs and Kinetic Alfven Waves." In Physics of Auroral Arc Formation, 451–55. Washington, D. C.: American Geophysical Union, 2013. http://dx.doi.org/10.1029/gm025p0451.

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8

Opher, Reuven. "Alfven Waves in Disks, Outflows and Jets." In Open Issues in Local Star Formation, 311–16. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/1-4020-2600-5_37.

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9

Califano, F., C. Chiuderi, and G. Einaudi. "A Case for Alfven Wave Heating." In Basic Plasma Processes on the Sun, 223–29. Dordrecht: Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-009-0667-9_36.

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10

Nocera, L., B. Leroy, and E. R. Priest. "Phase Mixing of Propagating Alfvén Waves." In Unstable Current Systems and Plasma Instabilities in Astrophysics, 365–69. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-6520-1_38.

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Тези доповідей конференцій з теми "Alfevn Waves"

1

Rauf, S., and J. A. Tataronis. "Four wave mixing of finite amplitude Alfven waves." In International Conference on Plasma Science (papers in summary form only received). IEEE, 1995. http://dx.doi.org/10.1109/plasma.1995.531714.

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2

Uberoi, C. "Alfven waves in space plasmas." In International conference on plasma physics ICPP 1994. AIP, 1995. http://dx.doi.org/10.1063/1.48998.

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3

Webb, G. M., Q. Hu, J. A. le Roux, B. Dasgupta, and G. P. Zank. "Double Alfvén waves." In PHYSICS OF THE HELIOSPHERE: A 10 YEAR RETROSPECTIVE: Proceedings of the 10th Annual International Astrophysics Conference. AIP, 2012. http://dx.doi.org/10.1063/1.4723593.

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4

de Azevedo, C. A., and A. .S. de Assis. "GLOBAL ALFVEN WAVES IN SOLAR PHYSICS." In 1st International Congress of the Brazilian Geophysical Society. European Association of Geoscientists & Engineers, 1989. http://dx.doi.org/10.3997/2214-4609-pdb.317.sbgf157.

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5

Stark, B. A., Z. E. Musielak, and S. T. Suess. "Alfvén wave resonances and flow induced by nonlinear Alfvén waves in a stratified atmosphere." In Proceedings of the eigth international solar wind conference: Solar wind eight. AIP, 1996. http://dx.doi.org/10.1063/1.51377.

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6

Valanju, P. M., R. D. Bengtson, W. D. Booth, R. W. Cook, T. E. Evans, S. M. Mahajan, M. E. Oakes, D. W. Ross, and Clifford M. Surko. "Alfven wave studies on PRETEXT." In AIP Conference Proceedings Volume 129. AIP, 1985. http://dx.doi.org/10.1063/1.35263.

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7

Thompson, B. J., and R. L. Lysak. "Magnetosphere-ionosphere coupling by inertial Alfven waves." In International Conference on Plasma Science (papers in summary form only received). IEEE, 1995. http://dx.doi.org/10.1109/plasma.1995.531677.

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8

Amagishi, Y., M. J. Ballico, R. C. Cross, and I. J. Donnely. "Discrete Alfven waves in the TORTUS tokamak." In Radio−frequency power in plasmas. AIP, 1989. http://dx.doi.org/10.1063/1.38479.

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9

Voitenko, Yu. "Note on dispersive Alfven waves in the solar corona." In Waves in dusty, solar and space plasmas. AIP, 2000. http://dx.doi.org/10.1063/1.1324954.

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10

Chen, Liu, and Fulvio Zonca. "Physics of Alfvén Waves." In Proceedings of the 12th Asia Pacific Physics Conference (APPC12). Journal of the Physical Society of Japan, 2014. http://dx.doi.org/10.7566/jpscp.1.011001.

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Звіти організацій з теми "Alfevn Waves"

1

W.W.Lee, J.L.V.Lewandowski, T.S. Hahm, and Z. Lin. Shear-Alfven Waves in Gyrokinetic Plasmas. Office of Scientific and Technical Information (OSTI), October 2000. http://dx.doi.org/10.2172/765443.

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2

Mahajan, S. M. Spectrum of Alfven waves, a brief review. Office of Scientific and Technical Information (OSTI), September 1995. http://dx.doi.org/10.2172/108117.

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3

O.Ya. Kolesnychenko, V.V. Lutsenko, and R.B. White. Ion Acceleration in Plasmas with Alfven Waves. Office of Scientific and Technical Information (OSTI), June 2005. http://dx.doi.org/10.2172/840913.

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4

Yoshida, Z., and S. M. Mahajan. Decay of magnetic helicity producing polarized Alfven waves. Office of Scientific and Technical Information (OSTI), February 1994. http://dx.doi.org/10.2172/10139403.

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5

Agim, Y., and S. Prager. Magnetic fluctuations due to thermally excited Alfven waves. Office of Scientific and Technical Information (OSTI), January 1990. http://dx.doi.org/10.2172/7185007.

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6

Johnson, J. R., and C. Z. Cheng. Kinetic Alfven waves and plasma transport at the magnetopause. Office of Scientific and Technical Information (OSTI), May 1997. http://dx.doi.org/10.2172/304098.

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7

I.Y. Dodin and N.J. Fisch. Alfven Wave Tomography for Cold MHD Plasmas. Office of Scientific and Technical Information (OSTI), September 2001. http://dx.doi.org/10.2172/788236.

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8

Cheng, C. Z., G. Y. Fu, and J. W. Van Dam. Toroidal Alfven wave stability in ignited tokamaks. Office of Scientific and Technical Information (OSTI), January 1989. http://dx.doi.org/10.2172/6386067.

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9

Campbell, R. B., and T. K. Samec. Alfven wave stability in D-III-D. Office of Scientific and Technical Information (OSTI), September 1989. http://dx.doi.org/10.2172/5146589.

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10

Berk, H. L., B. N. Breizman, and M. Pekker. Simulation of Alfven wave-resonant particle interaction. Office of Scientific and Technical Information (OSTI), July 1995. http://dx.doi.org/10.2172/101183.

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