Kinetic Alfvén wave in three-component dusty plasmas

Ac, Das; Misra, Arup Kumar; Ks, Goswami

doi:10.1103/physreve.53.4051

Cited by 27 publications

(12 citation statements)

References 13 publications

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“…͑22͒ for several parameters which are close to dusty plasma environments in interstellar clouds. [46][47][48] Interstellar dust make up only 1% of the interstellar medium but sometimes there is enough dust to obscure the light from stars behind the dust. The interstellar medium contains carbon, helium, hydrogen, and other gases such as oxygen, nitrogen, and baryonic gas molecules.…”

Section: Resultsmentioning

confidence: 99%

Kinetic Alfvén wave instability in a Lorentzian dusty magnetoplasma

et al. 2010

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This study presents a theoretical approach to analyze the influence of kappa distributed streaming ions and magnetized electrons on the plasma wave propagation in the presence of dust by employing two-potential theory. In particular, analytical expressions under certain conditions are derived for various modes of propagation comprising of kinetic Alfvén wave streaming instability, two stream instability, and dust acoustic and whistler waves. A dispersion relation for kinetic Alfvén-like streaming instability has been derived. The effects of dust particles and Lorentzian index on the growth rates and the threshold streaming velocity for the excitation of the instability are examined. The streaming velocity is observed to be destabilizing for slow motion and stabilizing for fast streaming motions. It is also observed that the presence of magnetic field and superthermal particles hinders the growth rate of instability. Possible applications to various space and astrophysical situations are discussed.

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Section: Resultsmentioning

confidence: 99%

Kinetic Alfvén wave instability in a Lorentzian dusty magnetoplasma

et al. 2010

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“…In a dustless plasma, i.e., ω pd ¼ 0, we obtain usual dispersion relation in electron-ion plasma. Expressing ω in terms of real and imaginary part, ω ¼ ω r þ iγ, with ω r >> γ, we either obtain growth or damping of KAW satisfying the condition, ω=k z ¼ v A ≤ v z through wave particle interactions [33,34]. In a dusty plasma with dust charge fluctuation effect, the main mechanism of wave damping is associated with dust charge fluctuation effects as compared to Landau damping [34].…”

Section: Kinetic Alfvén Waves In Maxwellian Plasmamentioning

confidence: 96%

“…The plasma beta β e is assumed to be very small. The electric field and the wave vector k lie in the xz plane, i.e., B 0 ¼ 0; 0; B 0ẑ ðÞ , V 0 ¼ 0; 0; V 0ẑ ðÞ , k ¼ k ⊥x ; 0; k zẑ ðÞ : We again solve the Vlasov equation For hot and magnetized electrons [33] to get the number and current density of electrons as obtained in the previous section. Making use of Eqs.…”

Section: Kaw and Instability In Lorentzian Plasmamentioning

confidence: 99%

Collective Mode Interactions in Lorentzian Space Plasma

Rubab¹,

Zaheer²

2018

Kinetic Theory

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Plasmas exhibit a vast variety of waves and oscillations in which moving charged particle produce fields which ultimately give rise to particle motion. These wave-particle effects are used in the acceleration heating methods of plasma particles, and in wave generation as well. Plasmas are often manipulated with EM waves, e.g., Alfvén waves are long-wavelength modes (drift-waves) where fluid theory is most reliable, while for short wavelength modes (e.g., Kinetic Alfvén waves), collisionless effects becomes important. In this chapter, the properties of kinetic Alfvén waves are aimed to study by employing two potential theory by taking particle streaming and Weibel instability with temperature anisotropy in a Lorentzian plasma.

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“…The damping of KAWs in dusty plasma has been studied rigorously by many authors. Das et al (1996) studied the KAW by retaining the finite Larmor radius of dust grains and showed that unlike MHD Alfvén waves, the KAW propagate across the magnetic field and because of its coupling to electrostatic modes, i.e., dust acoustic mode, and it undergoes Landau damping for each plasma species (Das et al, 1996) …”

Section: Damping Of Kinetic Alfvén Wavesmentioning

confidence: 99%

Alfvén waves in space and astrophysical dusty plasmas

Jatenco‐Pereira¹,

Chian

Rubab

2014

Nonlin. Processes Geophys.

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Abstract. In this paper, we present some results of previous works on Alfvén waves in a dusty plasma in different astrophysical and space regions by taking into account the effect of superthermal particles on the dispersive characteristics. We show that the presence of dust and superthermal particles sensibly modify the dispersion of Alfvén waves. The competition between different damping processes of kinetic Alfvén waves and Alfvén cyclotron waves is analyzed. The nonlinear evolution of Alfvén waves to chaos is reviewed. Finally, we discuss some applications of Alfvén waves in the auroral region of space plasmas, as well as stellar winds and star-forming regions of astrophysical plasmas.

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Kinetic Alfvén wave in three-component dusty plasmas

Cited by 27 publications

References 13 publications

Kinetic Alfvén wave instability in a Lorentzian dusty magnetoplasma

Kinetic Alfvén wave instability in a Lorentzian dusty magnetoplasma

Collective Mode Interactions in Lorentzian Space Plasma

Alfvén waves in space and astrophysical dusty plasmas

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