Waves in Complex Plasmas With Dust Distributions (Charge/Size/Mass) Revisited

Verheest, Frank; Cattaert, Tom

doi:10.1109/tps.2004.826086

Cited by 3 publications

(2 citation statements)

References 36 publications

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“…In line with previous work Verheest & Cattaert 2003, 2004 we write averages over the equilibrium dust distribution as…”

Section: General Remarksmentioning

confidence: 98%

“…As explained elsewhere (Verheest & Cattaert 2003) the different charge and mass weightings compel one to introduce a whole sequence of velocities and higher order moments, where the same order in w is combined with different powers of q/m, due to the magnetic part of the Lorentz force. To avoid these complications, we postpone the integration over these new phase space variables and restrict ourselves at first to integrations solely over the microscopic velocity w. More details about this half-way house procedure are given elsewhere (Verheest & Cattaert 2004), and we define the first two velocity moments of f d as…”

Section: Nonlinear Formalismmentioning

confidence: 99%

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Nonlinear electromagnetic modes in astrophysical plasmas with dust distributions

Verheest

Cattaert

2004

A&A

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Abstract.A derivative nonlinear Schrödinger equation is obtained for parallel electromagnetic modes in plasmas containing polydisperse charged dust. The coefficient of the dispersive term in that equation is dominated by the dust rather than the (plasma) ions, and polydisperse dust yields a larger coefficient in absolute value than an equivalent monodisperse description. This leads to a significant broadening of the nonlinear structure due to the presence of polydisperse rather than monodisperse dust, the latter contributing in itself already to a substantial increase in the width of envelope solitons compared to dust-free plasmas. When modelling the charged dust by a power-law distribution occurring in planetary ring and other astrophysical systems, it depends very much on the power-law index whether the smaller or the larger grains are more important. For certain indices the more numerous smaller grains determine the charge and mass densities, but the larger dust dominates the linear and nonlinear dispersive effects.

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“…In line with previous work Verheest & Cattaert 2003, 2004 we write averages over the equilibrium dust distribution as…”

Section: General Remarksmentioning

confidence: 98%

Section: Nonlinear Formalismmentioning

confidence: 99%

Nonlinear electromagnetic modes in astrophysical plasmas with dust distributions

Verheest

Cattaert

2004

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Nonlinear electrostatic modes in astrophysical plasmas with charged dust distributions

Verheest

Yaroshenko

2009

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Context. Most theoretical investigations of wave phenomena in dusty plasmas have treated charged dust as additional heavy negative ions in standard multispecies models. Many dusty plasma experiments use monodisperse grains, but charged (and neutral) grains in space environments come in a whole range of sizes and compositions, hence in masses and charges. Dust density distributions having a power-law decay with size are often observed in planetary rings. Aims. There is a need to investigate larger solitary structures, since wave descriptions involving charged dust distributions have usually been limited to linear or weakly nonlinear modes. Methods. Sagdeev pseudopotential methods describe large-amplitude solitary waves in a co-moving reference frame and are adapted to include dust distributions, using mass and charge, or alternatively size, as additional variables. Observed power-law distributions lead to descriptions involving hypergeometric functions. Results. Lower limits for possible solitary wave velocities follow from requiring that the Sagdeev pseudopotentials have a local maximum for the undisturbed conditions, whereas upper limits come from ensuring that dust densities remain real. Nonlinear amplitudes increase with solitary wave velocities and relative electron temperature. Under similar plasma conditions, dust size distributions admit slower solitary wave solutions, with correspondingly smaller amplitudes than given by monodisperse dust models. For typical planetary ring conditions, the difference can be quite appreciable.

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Dispersion relation for pure dust Bernstein waves in a non-Maxwellian magnetized dusty plasma

2011

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Pure dust Bernstein waves are investigated using non-Maxwellian kappa and (r,q) distribution functions in a collisionless, uniform magnetized dusty plasma. Dispersion relations for both the distributions are derived by considering waves whose frequency is of the order of dust cyclotron frequency, and dispersion curves are plotted. It is observed that the propagation band for dust Bernstein waves is rather narrow as compared with that of the electron Bernstein waves. However, the band width increases for higher harmonics, for both kappa and (r,q) distributions. Effect of dust charge on dispersion curves is also studied, and one observes that with increasing dust charge, the dispersion curves shift toward the lower frequencies. Increasing the dust to ion density ratio (nd0ni0) causes the dispersion curve to shift toward the higher frequencies. It is also found that for large values of spectral index kappa (κ), the dispersion curves approach to the Maxwellian curves. The (r,q) distribution approaches the kappa distribution for r = 0, whereas for r > 0, the dispersion curves show deviation from the Maxwellian curves as expected. Relevance of this work can be found in astrophysical plasmas, where non-Maxwellian velocity distributions as well as dust particles are commonly observed.

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Waves in Complex Plasmas With Dust Distributions (Charge/Size/Mass) Revisited

Cited by 3 publications

References 36 publications

Nonlinear electromagnetic modes in astrophysical plasmas with dust distributions

Nonlinear electromagnetic modes in astrophysical plasmas with dust distributions

Nonlinear electrostatic modes in astrophysical plasmas with charged dust distributions

Dispersion relation for pure dust Bernstein waves in a non-Maxwellian magnetized dusty plasma

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