Non-linear interaction of the kinetic Alfvén waves   and the filamentation 
process in the solar wind plasma

Sharma, R. P.; Malik, M.

doi:10.1051/0004-6361:20054715

Cited by 7 publications

(4 citation statements)

References 37 publications

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“…Most of the work related to filamentation is done in the framework of Hall MHD [21]. The Nonlinear interaction of kinetic Alfvén waves with Gaussian perturbation and the turbulent spectrum due to filamentation have been studied [22]. These structures are originated because of the nonlinear interactions and are responsible for the energy transfer from the injection scales to the smaller scales, until dissipative effects due to Landau damping become dominant and stop the energy cascade.…”

Section: Resultsmentioning

confidence: 99%

Landau damped kinetic Alfvén waves and coronal heating

Sharma¹,

Kumar²

2009

J. Plasma Phys.

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Some recent observations of solar corona suggest that the kinetic Alfvén waves (KAWs) turbulence may be responsible for electron acceleration in solar corona and coronal heating. In the present research, we investigate the turbulent spectra of KAW due to filamentation process in the presence of Landau damping and particle energization. We present here the numerical simulation of model equation governing the nonlinear dynamics of the KAW in the presence of Landau damping. When the ponderomotive and Joule heating nonlinearities are incorporated in the KAW dynamics, the power spectra of the turbulent field is evaluated and used for particle heating. Our results reveal the formation of damped coherent magnetic filamentary structures and the turbulent spectra. The effect of Landau damping is to make the turbulent spectra steeper. Two types of scalings k −3.6 and k −4 have been obtained. We have studied the turbulence with different initial conditions. Using the Fokker-Planck equation with the new velocity space diffusion coefficient, we find the distribution function of energetic electrons in these turbulent structures. Landau damped KAWs may be responsible for the acceleration of the energetic electrons in solar corona and coronal heating.

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Section: Resultsmentioning

confidence: 99%

Landau damped kinetic Alfvén waves and coronal heating

Sharma¹,

Kumar²

2009

J. Plasma Phys.

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“…They proposed the necessities of more theoretical work in this direction in future to understand these processes. Besides this, Shukla and Sharma [2001] and recently, Sharma and Malik [2006] have also studied the mutual nonlinear interaction between two kinetic Alfvén beams and the effect on filament formation process. When the two KAWs are present, the background density modification by ponderomotive nonlinearities depends on the intensity of both the KAWs (in contrast to single coherent beam case) and the filamentation threshold is considerably reduced by increasing the power of the second beam.…”

Section: Discussionmentioning

confidence: 95%

Alfvén wave filamentation and particle acceleration in solar wind and magnetosphere

2006

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[1] We present numerical simulations of Alfvén waves in steady state, leading to the formation of intense magnetic filaments when the nonlinearity arises due to the ponderomotive effects and Joule heating. When the plain Alfvén wave is perturbed by a transverse perturbation and the magnitude of the pump Alfvén wave changes, chaotic filamentary structures of magnetic field in kinetic Alfvén wave (KAW) filamentation and quasiperiodic in inertial Alfvén wave (IAW) filamentation have been observed. At higher KAW pump wave amplitude, the spectra approaches near the Kolmogorov k À5/3 scaling. The spectral index becomes k À3 scaling in IAW. Relevance of these studies in solar wind and magnetosphere for KAW and solar corona and auroral region for IAW has also been pointed out. Particle heating in these small-scale filamentary structures has also been calculated by using velocity space diffusion coefficient in Fokker-Planck equation.Citation: Sharma, R. P., H. D. Singh, and M. Malik (2006), Alfvén wave filamentation and particle acceleration in solar wind and magnetosphere,

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“…Since discovered in the 1970s [ Chen and Hasegawa , ; Hasegawa and Chen , , ], KAWs have been attracting the attention of researchers in the fields of astrophysical, space, and laboratory plasmas. Specifically, they have been applied to the inhomogeneous heating of coronal magnetoplasma fine structures [ Wu and Fang , ], the acceleration of terrestrial auroral electrons [ Wu and Chao , ], the dissipation of solar wind turbulence [ Sridhar and Goldreich , ; Goldreich and Sridhar , ; Salem et al , ], the formation of magnetoplasma fine structures [ Malik and Sharma , ; Sharma and Malik , ; Brodin et al , ; Malik et al , ; Singh and Sharma , ] and the zonal flow phenomena in laboratory plasmas [ Vlad et al , ].…”

Section: Introductionmentioning

confidence: 99%

“…KAWs always occur with strongly transverse density fluctuations because of their strong anisotropy and coupling with small‐scale electrostatic modes. The nonlinear dynamics and evolution of coupling KAWs are studied by Sharma and Malik [] and Singh and Sharma []; they found that the nonlinear interaction of KAWs can lead to the spatial amplification and the filament formation ultimately. They also pointed out that these filamentary structures can play an important role in the coronal heating and the solar wind acceleration/turbulence.…”

Section: Introductionmentioning

confidence: 99%

A possible mechanism for the formation of filamentous structures in magnetoplasmas by kinetic Alfvén waves

Chen

Zhao

et al. 2015

JGR Space Physics

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Due to having strong anisotropy in their polarization state and spatial structure, it is believed that kinetic Alfvén waves (KAWs) can play an important role in various energization phenomena of plasma particles and the fine-structure formation in magnetoplasma environments. The filamentous fine structures are a kind of the common density inhomogeneity phenomena in magnetoplasmas, and hence, the density gradient is one of the sources of free energy that can lead to KAWs instabilities. In this paper, based on the two-fluid model in which ions and electrons are treated as separate fluids, we investigate the effect of density gradient inhomogeneous on the dispersion and instability of KAWs in a magnetoplasma. The results show that KAW instability can be excited effectively by the density gradient. Especially, both the real frequency R and the growth rate I of KAWs are dramatically dependent on the spatial position x in the presence of an inhomogeneous density gradient. The results also show that the real frequency increases with the characteristic spatial scale of inhomogeneity, while the growth rate of KAWs has a maximum in the growing ranges of. On the other hand, the excited KAWs are weakly dispersive with e k x < 1. The results have potential importance for a better understanding of the microphysics of the filamentous fine-structure formation since the phenomena of density gradient inhomogeneous are ubiquitous in various magnetoplasmas, such as in the laboratory plasma as well as in both the solar coronal and terrestrial auroral plasmas.

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Non-linear interaction of the kinetic Alfvén waves and the filamentation process in the solar wind plasma

Cited by 7 publications

References 37 publications

Landau damped kinetic Alfvén waves and coronal heating

Landau damped kinetic Alfvén waves and coronal heating

Alfvén wave filamentation and particle acceleration in solar wind and magnetosphere

A possible mechanism for the formation of filamentous structures in magnetoplasmas by kinetic Alfvén waves

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