Magnetorotational instability in dissipative dusty plasmas

Ren, Haijun; Wu, Zhengwei; Chu, Paul K.

doi:10.1063/1.3272092

Cited by 8 publications

(5 citation statements)

References 70 publications

(69 reference statements)

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“…Eliminating the perturbations from Eqs. (18) and (19), the local dispersion relation of the MRI in magnetized plasmas with mobile dust grains is…”

Section: Local Dispersion Relationmentioning

confidence: 99%

“…Theoretical analyses were first performed by Mikhailovskii et al 16 who studied MRI in a dusty plasma utilizing the one-fluid MHD approach generalized to include the immobile dust effects. 18,19 Here, the dust grains were assumed to be heavy enough to be immobile so that the dust effects were contained in the model only by introducing an electric field term in the onefluid equation of plasma motion. It should be noted that most studies have adopted the one-fluid model in the analytical study of MRI and the two-fluid model has been proposed recently by Ren et al 20 More recently, Ren et al investigated the MRI in a weakly ionized plasma by taking into account collisions between neutrals and the plasma.…”

Section: Introductionmentioning

confidence: 99%

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Magnetorotational instability in plasmas with mobile dust grains

Ren¹,

Li²,

Chu³

2013

Physics of Plasmas

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The magnetorotational instability of dusty plasmas is investigated using the multi-fluid model and the general dispersion relation is derived based on local approximation. The dust grains are found to play an important role in the dispersion relation in the low-frequency mode and exhibit destabilizing effects on the plasma. Both the instability criterion and growth rate are affected significantly by the dust and when the dust is heavy enough to be unperturbed, the reduced dispersion relations are obtained. The instability criteria show that the dust grains have stabilizing effects on the instability when the rotation frequency decreases outwards and conversely lead to destabilizing effects when the rotation frequency increases outwards. The results are relevant to accession and protoplanetary disks. V

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“…Eliminating the perturbations from Eqs. (18) and (19), the local dispersion relation of the MRI in magnetized plasmas with mobile dust grains is…”

Section: Local Dispersion Relationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Magnetorotational instability in plasmas with mobile dust grains

Ren¹,

Li²,

Chu³

2013

Physics of Plasmas

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“…MRI is also expected to act as a dynamo in the accretion disks 67 . Hereinafter, there is a growing interest in MR instability applications concerning the astrophysical problems in various magnetized accretion disks 68 – 70 . Different models, various analytical explanations and numerical analysis has been performed to explain the dynamics of MRI in different situations i.e., Single 63 and two fluid model 71 was developed with effect of magnetized and un-magnetized plasma, The effect of viscosity in rotating plasma 72 and rotating dusty plasmas including dissipation 73 .…”

Section: Introductionmentioning

confidence: 99%

Magnetorotational instability in dense electron–positron–ion plasmas

Usman,

Mushtaq

2023

Sci Rep

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We in this manuscript analyzed the magnetorotational instability (MRI) by using a multi-component quantum fluid model with the effect of spin magnetization in a differentially rotating degenerate electron–positron–ion (e–p–i) quantum plasma. The electrons and positron having the same mass but opposite charge are taken to be degenerate whereas ions are considered as classical owing to their large inertia. The general dispersion relation is derived and a local dispersion relation for MRI is obtained by applying MHD approximations. To obtained MRI and to analyze the results numerically, reduced dispersion relation is derived using the local approximations. The obtained results are applied to the astrophysical situations exist there in the interiors of White Dwarfs and neutron stars. Contribution from spin magnetization and the number densities of electrons and positrons plays a vital role in the dynamics and can alter the instability. The increase in the electron number density, hence spin magnetization enhances the growth rate of the mode and leads the system to instability which results in the core collapse of certain massive stars.

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“…Magnetorotational instability (MRI), also known as Velikhov–Chandrasekhar instability, which is a feature of purely rotating fluids, was investigated in a differentially rotating dusty plasma where the dust particles were considered fixed. [ 28 ] Very recently, Hartmann et al [ 29 ] studied both experimentally and with molecular dynamics simulations the self‐diffusion phenomenon in a 2D dusty plasma, where experimentally a high magnetic field was created with the rotation of the dust grain cloud.…”

Section: Introductionmentioning

confidence: 99%

Shock waves in a rotating non‐Maxwellian viscous dusty plasma

Ehsan

Abbasi

Ghosh

et al. 2020

Contributions to Plasma Physics

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A theoretical model is presented to study the characteristics of dust acoustic shock in a viscous, magnetized, rotating dusty plasma at both fast and slow time scales. By employing the reductive perturbation technique, the non-linear Zakharov-Kuznetsov-Burger (ZKB) equation is derived for both cases when the dust is inactive and dynamic (fast and slow time scales). Both electrons and ions are considered to follow the kappa/Cairns distribution. It is observed that in both cases, i.e. when dust is in the background and active, viscosity plays a key role in dissipation for the propagation of acoustic shock. Magnetic field and rotation are responsible for the dispersive term. Superthermality is found to affect significantly the formation of the shock wave along with viscous nature of plasma, whereas the dust charge affects the non-linear coefficient of the ZKB equation. The present investigation may be beneficial to the understanding of the rotating plasma, in particular the experiments being carried out. K E Y W O R D S dusty plasmas, nonlinear waves, shocks, ZK Burger equation 1 INTRODUCTION Despite a history spanning nearly a century, research into complex (dusty) plasmas (consisting of solid particles of nanometres to hundreds of micrometres size in a conventional two-component plasma) has progressed significantly only in last two decades, mainly after the marvellous observation of dusty plasma crystals by Thomas et al. in 1994. [1] Also, for more than 10 years dusty plasmas under minute gravity conditions have been studied on board the International Space Station (ISS) under the joint Russian/German venture of Plasma Kristall (PK), along with PKE-Nefedov, PK-3 Plus, and PK-42014 onwards. [2] Other than novel experimental discoveries of dusty plasma crystals, dust Mach cones, [3] dust acoustic waves, dust voids, [4] etc., the notion of possible existence of 'dust atoms and molecules' was also put forward by Tsintsadze, Murtaza, and Ehsan. [5] The authors later reported the crystallization of dust atoms in the localized region of the electromagnetic wave. [6] The importance of dusty plasma physics has been manifold, because such plasmas are omnipresent in astrophysical environment like comets, interplanetary or interstellar clouds, the rings of giant planets like Saturn, etc., whereas

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Magnetorotational instability in dissipative dusty plasmas

Cited by 8 publications

References 70 publications

Magnetorotational instability in plasmas with mobile dust grains

Magnetorotational instability in plasmas with mobile dust grains

Magnetorotational instability in dense electron–positron–ion plasmas

Shock waves in a rotating non‐Maxwellian viscous dusty plasma

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