A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layers: Part I. Basic mechanism

Hoshoudy, G. A.; Çavuş, Hüseyin; Mahdy, A.

doi:10.1007/s10509-019-3576-2

Cited by 3 publications

(5 citation statements)

References 29 publications

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“…In present work, the fundamental goal is to investigate the influences of B-field, ΔU, T, kI and k on the γ of the magnetized KHI with continuous profiles through a viscous medium in the solar atmosphere using the model of Hoshoudy, Cavus and Mahdy(2019). In this investigation, decisive values of B-field, ΔU, T and k in the solar atmosphere captured from the graphs.…”

Section: Discussionmentioning

confidence: 99%

“…Under the aforementioned assumptions, equations, that are (Wang et. al., 2009 andYe et al, 2011;Hoshoudy, Cavus and Mahdy;2019)  …”

Section: Fundamental Physics and Mathematicsmentioning

confidence: 99%

“…These equations are nonlinear and analytical solutions are difficult to obtain. We shall continue as in Hoshoudy, Cavus and Mahdy (2019). In our study, we consider the motion in two-dimensional ) , ( y x , where the two-dimensional disturbances are more unstable than threedimensional which is proved by Squire's theorem (Todd et al, 1986).…”

Section: Fundamental Physics and Mathematicsmentioning

confidence: 99%

“…The leading goal of this paper is to make an investigation of magnetohydrodynamic KHI with continuous profiles through a viscous medium in the solar atmosphere. The model of Hoshoudy, Cavus and Mahdy (2019) will be used as a method. The mathematics used in this work is given in the next section.…”

mentioning

confidence: 99%

“…

The main aim of this submission is to investigate the effects of some parameters like wave number, shear velocity, magnetic field and temperature for the growth rate of the magnetized Kelvin-Helmholtz instability (KHI) with incessant profiles through interface of two viscous fluid layer occurred in the solar atmosphere using the model of Hoshoudy, Cavus and Mahdy (2019). In this examination, the presence of KHI is identified for the various cases of wave number, magnetic field, shear velocity and temperature in the solar atmosphere.

…”

mentioning

confidence: 99%

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A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layer: Part II. An application to the atmosphere of the Sun

Çavuş

Hoshoudy

2019

Astrophys Space Sci

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Section: Discussionmentioning

confidence: 99%

“…Under the aforementioned assumptions, equations, that are (Wang et. al., 2009 andYe et al, 2011;Hoshoudy, Cavus and Mahdy;2019)  …”

Section: Fundamental Physics and Mathematicsmentioning

confidence: 99%

Section: Fundamental Physics and Mathematicsmentioning

confidence: 99%

mentioning

confidence: 99%

“…

…”

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confidence: 99%

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A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layer: Part II. An application to the atmosphere of the Sun

Çavuş

Hoshoudy

2019

Astrophys Space Sci

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Effects of head loss, surface tension, viscosity and density ratio on the Kelvin–Helmholtz instability in different types of pipelines

Yang

Cao

2021

Physica D: Nonlinear Phenomena

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Instability of three dimensional electrically conducting fluid of magnetohydrodynamics Couette flow

Hussain

Elazab²,

Hussain

et al. 2019

AIP Advances

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In this work, we consider a disturbed electrically conductive fluid between two parallel planes and study the stability of the fluid after applying a uniform magnetic field on it. We obtain a modified form of Orr-Sommerfeld system of equation and then use QZ (Qualitat and Zuverlassigkeit) technique to obtain neutral curves. We investigate the critical Reynolds numbers for large domain of Hartmann Number. Next we show that for particular values of oblique angle, Couette flow destabilizes in some range of magnetic field. We also show that the area of stability changes with change oblique angle, Hartmann number, Reynolds number and wave number. We also find that the instability region for Couette flow has conic type shape. It is found that magnetic field provides a stabilizing impact to the flow, and the extent of this impact is demonstrated for a range of Reynolds numbers. From numerical simulations, it is observed that a magnetic field with a specific magnitude stabilizes the Hartmann flow.

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A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layers: Part I. Basic mechanism

Cited by 3 publications

References 29 publications

A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layer: Part II. An application to the atmosphere of the Sun

A viscous magnetohydrodynamic Kelvin–Helmholtz instability in the interface of two fluid layer: Part II. An application to the atmosphere of the Sun

Effects of head loss, surface tension, viscosity and density ratio on the Kelvin–Helmholtz instability in different types of pipelines

Instability of three dimensional electrically conducting fluid of magnetohydrodynamics Couette flow

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