The Physics of Alfvén Waves

Cramer, N. F.

doi:10.1002/3527603123

Cited by 181 publications

(154 citation statements)

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“…For a model description of the spatial structure of the excited wave field, a standard Hall-MHD description is chosen [24]. Collisional effects are taken into account by including the perpendicular resistivity η in the generalized Ohm's law…”

Section: Wave Polarizationmentioning

confidence: 99%

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Alfvén wave dispersion behavior in single- and multicomponent plasmas

et al. 2010

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Section: Wave Polarizationmentioning

confidence: 99%

“…We compare the experimental results with numerical calculations based on a multi-fluid Hall-MHD model including perpendicular resistivity. Together with Maxwell's equations, a plane wave ansatz leads to the dispersion equation in a cold uniform plasma [24]:…”

Section: Introduction and Basicsmentioning

confidence: 99%

Alfvén wave dispersion behavior in single- and multicomponent plasmas

et al. 2010

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“…In this case, we have c 4 ¼ 3/(1 À a À3 m ). The wave propagation in dusty plasma is modified, and some new and interesting effects take place (Wardle & Ng 1999;Cramer 2001). The dispersion relation of the Alfvén waves with frequencies smaller than the ion cyclotron frequency, considering dust particles with constant charges in a neutral and cold dusty plasma, is given by (Cramer et al 2002) …”

Section: Dust-cyclotron Dampingmentioning

confidence: 99%

The Effects of Alfven Waves and Radiation Pressure in Dusty Winds of Late‐Type Stars. II. Dust‐Cyclotron Damping

Vidotto¹,

Jatenco‐Pereira²

2006

ApJ

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There are in the literature several theories to explain the mass loss in stellar winds. In particular, for late-type stars, some authors have proposed a wind model driven by an outward-directed flux of damped Alfvén waves. The winds of these stars present great amounts of dust particles that, if charged, can give rise to new wave modes or modify the preexisting ones. In this work, we study how dust can affect the propagation of Alfvén waves in these winds, taking into account a specific damping mechanism, dust-cyclotron damping. This damping affects the Alfvén wave propagation near the dust-cyclotron frequency. Hence, if we assume a dust size distribution, the damping occurs over a broad band of wave frequencies. In this work, we present a model of Alfvén wave-driven winds using the dust-cyclotron damping mechanism. On the basis of coronal holes in the Sun, which present a superradial expansion, our model also assumes a diverging geometry for the magnetic field. Thus, the mass, momentum, and energy equations are obtained and then solved in a self-consistent approach. Our results of wind velocity and temperature profiles for a typical K5 supergiant star show compatibility with observations. We also show that, considering the presence of charged dust particles, the wave flux is less damped due to dust-cyclotron damping than it would be if we were to consider some other damping mechanisms studied in the literature, such as nonlinear damping, resonant surface damping, and turbulent damping.

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“…[28]). In this context, since the two equations (10) and (11) were substituted into (12), the assumption (9) implies that terms of the order Ω …”

Section: The Eigenmode Equationmentioning

confidence: 99%

Compressional Alfvén eigenmode structure in spherical tokamaks

Smith¹,

Verwichte

2009

Plasma Phys. Control. Fusion

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Abstract. The two-dimensional structure of compressional Alfvén eigenmodes below the ion cyclotron frequency is studied numerically by solving the cold plasma Hall-MHD equations for a realistic spherical tokamak equilibrium. The simplest of the computed eigenmodes have a standing wave-like structure and the higher frequency solutions show a more travelling wave-like behaviour. The effects of the equilibrium current and the Hall terms in the eigenmode equation are investigated, and these terms are found to shift the frequencies of eigenmodes with different sign of the toroidal mode number away from each other. A classification scheme is proposed which relates each spherical tokamak eigenmode to the three mode numbers of the corresponding large aspect ratio circular cross section eigenmode obtained by gradually decreasing the elongation and increasing the aspect ratio.

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The Physics of Alfvén Waves

Cited by 181 publications

References 0 publications

Alfvén wave dispersion behavior in single- and multicomponent plasmas

Alfvén wave dispersion behavior in single- and multicomponent plasmas

The Effects of Alfven Waves and Radiation Pressure in Dusty Winds of Late‐Type Stars. II. Dust‐Cyclotron Damping

Compressional Alfvén eigenmode structure in spherical tokamaks

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