Rayleigh-Taylor Instability of Magnetized Plasma through Darcy Porous Medium

Effects of horizontal and vertical magnetic field components on the Rayleigh-Taylor instability of stratified incompressible plasmas layer of variable density through Darcy porous medium are studied. The basic magnetohydrodynamic (MHD) set of equations has been constructed and linearized. Then the linear normalized growth rate is obtained analytically as a function of the physical parameters of the system considered. Numerical calculations have been performed to see the effects of various parameters on the normalized growth rate of Rayleigh-Taylor instability. It is found that the parameter D L λ λ ∗ = ( λ is constant and D L is the density-scale length) has an important role on the happening stability, where the maximum instability comes at 0.5 λ ∗ = − and to get more stable model we select λ ∗ through the region or 0.5 0.5 ∗ ∗ − < < − λ λ . The system will be more stable for the positive values of λ ∗ .


Introduction
The hydromagnetics stability of a magnetized plasma of varying density is of considerable importance in several astrophysical situations such as supernova explosions, in heating in solar corona, theories of sunspot magnetic fields, the formation and mixing of clouds and the stability of the stellar atmospheres in magnetic fields.The classical study of the equilibrium of an incompressible, inviscid fluid of variable density was first undertaken by Rayleigh [1], and later applied to all accelerated fluids by Taylor [2].Rayleigh showed the equilibrium of a horizontal layer of incompressible, ideal fluid is stable or unstable according as the density increases or de-creases anywhere in the vertically upward direction.Since then the problem is called Rayleigh-Taylor instability (RTI).RTI occurs naturally in many phenomenons of astrophysics, geophysics, and laboratories.It derives its character from the adverse density distribution of the matter, where the investigation of Rayleigh-Taylor instabilities in a magnetized plasma is a problem of considerable interest in space (ionospheric spread-F), fusion (curvature induced instabilities like interchange, ballooning, etc.) and the astrophysical plasmas.
Under various physical effects, the Rayleigh-Taylor instability problem of a finite layer of a fluid has been studied by several authors in hydrodynamics and in magnetohydrodynamics domain; the stabilizing effect of magnetic field on RTI problem for an incompressible plasma has been demonstrated by Kruskal and Schwarzschild [3] for a horizontal orientation of the magnetic field and by Hide [4] for a vertical orientation.The effects of viscosity and compressibility on the RTI of stratified plasma in the presence of magnetic field have been studied by Bhatia [5].The RTI in a rotating plasma of variable density including simultaneously the effects of viscosity and the finiteness of the ion Larmor radius have been investigated by Bhatia and Steiner [6].The effect of Hall current and finite electrical resistivity on the RTI of viscous, incompressible, finitely conducting plasma in a downward gravitational field under the influence of a uniform magnetic field normal to gravity has been studied by Kamla and Srivastav [7].The RTI of an infinitely conducting stratified dusty plasma medium including the effects of FLR corrections in the presence of a horizontal magnetic field has been studied by Kamal and Chhajlani [8].The RTI of a plasma layer in the presence of a horizontal magnetic field is investigated, taking into account the effects of Hall-currents and an arbitrarily large density gradient by Donald [9].The effects of Hall currents and viscosity on the RTI of an incompressible infinitely conducting stratified plasma permeated by a two-dimensional horizontal magnetic field have been investigated by Ahsan and Bhatia [10].The effects of Hall currents on the RTI of a finitely conducting stratified partially ionized plasma, where the plasma is permeated by a two dimensional horizontal magnetic field have been studied by Aiyub and Bhatia [11].In the presence of magnitude of the gravitational acceleration, the RTI of stratified incompressible plasma has been studied by Goldston and Rutherford [12].The RTI in the presence of horizontal magnetic field of incompressible plasma has been studied by Wu et al. [13].
The RTI of magnetized plasma through porous medium problem has a great scientific interest, where this problem corresponds physically (in astrophysics) to the Rayleigh-Taylor instability of an equatorial section of a planetary magnetosphere or of a stellar atmosphere where the magnetic field is perpendicular or parallels to gravity.So, the RTI of a stratified plasma through porous medium in the presence or absence of magnetic field has been studied by a number of researchers (Chhajlani and Vaghela, Vyas and Chhajlani, Sharma and Bhardwaj, Sharma and Sharma, Sharma and Trilok, Sharma and Sunil, Shikha and Bhatia, Opara, Sharma and Sunil, Sunil and Sharma, Sharma and Thakur and Sharma and Rajput).In this case (Darcy's model), the usual viscous term in the equation of motion is replaced by the resistive term , where µ is the fluid viscosity, 1 k is the medium permeability and a U is the Darcian (filter) velocity of the fluid.In all the above-mentioned studies, the behaviour of growth rates is considered with respect to the porosity of porous medium and the medium permeability in the presence of an variable magnetic field in x − direction only or in z − direction only.Here, we will discuss the role of resistive term (Darcy's term) besides the components of magnetic field in both x − and z − direction on growth rates of RTI of plasma layer

Formulation of the Problem
We consider the strata of incompressible and inviscous plasma as a fluid of electrons and immobile ions through Darcy porous medium in the presence of magnetic field B , where the relevant equations may be written, respectively (see references [12]- [25]), ( ) For incompressible flow the fluid elements move without changing density is to say that the Lagrangian total derivative of density is zero, that is (see reference [1]) where U is the velocity of the fluid, ρ is the density, p thermal pressure, e µ magnetic permeability, 0 µ coefficient of dynamic viscosity and g is the gravitational acceleration.One can see that the set of Equations ( 1)-( 4) is complete for describing the magnetic field effects on the R-T instability of incompressible plasma, since its number of equations exactly equals its number of unknown quantities: Two unknown vector quantities U and B and two unknown scalar quantities P and ρ .For the equilibrium profiles can be expressed in the form ( ) ( ) ( ) ( ) e .Now, we assume a small perturbation in the system of Equations ( 1)-( 4), where the perturbations in the velocity U , pressure p , magnetic field B , and density ρ , respectively, are ( ) , , , p p z p x y z t = + , ( ) ( ) , , , z x y z t . Then, the linearized equations can be easily derived from Equations ( 1)-( 4) in the form ( ) ( ) , , , , and the fluid is arranged in horizontal strata, then 0 ρ is a function of the vertical coordinate z only (i.e.

( )
) and ( ) ( ) Then the system of Equations ( 4)-( 8) become ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) If we assume that the perturbation in any physical quantity takes the form where x k and y k are horizontal components of the wave-number vector k such that 2 and ω (may be complex ( ) ) is the frequency of perturbations or the rate at which the system departs from equilibrium thee initial state.Using the expression (15) in the system of Equations ( 9)-( 14), we have ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) ( ) Now, if we eliminate some of the variables from the system of Equations ( 16)-( 21), we have a differential equation in 1

A Continuously Stratified Plasma
In this section we consider the case of incompressible continuously stratified plasma layer of thickness h con- fined between two rigid boundaries, in which the density and magnetic field distribution are given, respectively, by ( ) ( ) ( ) where ( ) ( ) and by substituting in Equation ( 24), we will have an equation in both π sin n z h respectively, are given by: Now, we define the dimensionless quantities x z Then Equations ( 25) and (26), respectively, take the form { } ( ) Now, we put i r ω ω γ * * = + and for 0 r ω * = (stable oscillations), then Equations ( 28) and ( 29) may be given by: Now, if we rearrange the above two equations (Equations ( 30) and ( 31)), we will have From Equations ( 32) and (33) maybe we can specialize the next special cases: (i) In the case of λ * = − , and substituting in Equation ( 32) we find that the normalized growth rate given by 2 Goldston and Rutherford 2 2 This case is considered by Goldston and Rutherford (see reference [12]).(ii) In the case of λ * = − , and substituting in Equation ( 32), then the normalized growth rate given by This case studied in reference [12].It is clarified that, the horizontal magnetic field has stabilizing effect on RTI problem.This influence is obvious from Equations (34) and ( 35 λ * = − , and substituting in Equation (32), the normalized growth rate given by Now, comparing between Equations (34) and (36), someone can observe that, the stabilizing role for the vertical magnetic field on the considerable system, where vertical magnetic field λ * = − , and substituting in Equation (32), the dispersion rate given by { } Then, the normalized growth rate becomes From Equations (34) and (38) it is very clear that, Darcy Goldston and Rutherford γ γ < .
The stabilizing effects of the horizontal, vertical magnetic and resistive term, unaccompanied, (above cases (i)-(iv)) on the RTI have been numerically presented in Figure 1.
(v) For the general case ( 2 2 0, 0 between Equations (32) and (33) the normalized dispersion relation takes in the form.
In this case the normalized growth rate given as. where In fact, the square of normalized growth rate 2 γ in Equation ( 40) is a function in the dimensionless quanti- ties of horizontal ( ) are the parameters of problem that maybe take a different values.But the constant λ * is unknown in the general case (v), while in the absence of magnetic field or in the presence of either them (horizontal or vertical magnetic field components) we note that 1 2 λ * = − (special cases (i)-(iv)).So, firstly we will discuss the role of constant λ * on the square of normalized growth rate 2 γ in the presence of horizontal, vertical magnetic field components and re- sistive term.
The role of constant λ * in the presence of both horizontal and vertical magnetic field components   γ decrease while the magnitude of λ * increases.
These implies that the maximum instability in the presence of both horizontal and vertical components of magnetic field happens at 0.5 (in the presence or absence of resistive term).The general case (Equation (40)), that gives the effects of horizontal, vertical magnetic field and resistive term together on the instability of the considered system has been presented in λ * = − (maximum instability) the system of Equations ( 39)-(43) take the form:     to the left or right hand, the system tends to stability.In closing this paper, the Rayleigh-Taylor instability in stratified plasma in the presence of combined effect of horizontal and vertical magnetic field through Darcy porous medium is considered.The solution of the system leads to a dispersion relation where the physical parameters are put in the dimensionless form.Some special cases are particularized to explain the roles that play the variables of the problem and numerical solutions are made.Some stability diagrams are plotted and discussed.The results show that, as the growth rate depends on the horizontal and vertical components of magnetic field and resistive term (Darcy's term) also depends on the parameter D L λ λ * = .Numerically the maximum instability (normalized growth rate) happens at 0.5 and then analytically the maximum instability gives in Equation (45).The system will be more stable if we select λ * such that to be different than −0.5.Finally, for the behavior of our selected system with respect to the parameter λ * we have not clear interpreting at this stage.
( λ is constant and D L is the density-scale length) has an important role on the happening stability, where the maximum instability comes at 0.5 λ * = − and to get more stable model we select λ * through the region or 0 density-scale length) are constants, then Equation (22) takes the form and Darcy 0 ω * = A second time, from Equation (33) we get 1 2

Figure 1 .
Figure 1.The role of parameter's problem, unaccompanied, where the square normalized growth rate ( ) 2 γ against and vertical ( ) z f ω * components of the magnetic field, the dimensionless resistive term Darcy (ω * , dimensionless Darcy term ) , the wave number k * and λ * ( D L λ λ * = , where λ is constant and D L is the density-scale length).The dimensionless quantities

is plotted in Figure 2 ,
where the square normalized growth

Figure 2 .
Figure 2. The role of constant λ * on the 2 γ in the presence of 0.4 x z f f ω ω * * = = and the resistive term Darcy 0.3 ω * = through the range

. 2 γ
For the values λ * that is less than see that, the magnitude of decrease with decreasing of λ * .For the values λ *

Figure 3 . 2 γ. 2 γ
where the square normalized growth rate is plotted against the square normalized wave number2   Second time, one can see that, the maximum instability (maximum square normalized growth rate

Finally, Figure 4
Shows the role of constant λ * , where the maximum happens at 0.5 λ * = − .If we move

Figure 3 . 2 γ against the square normalized wave number 2 k
Figure 3.The square normalized growth rate ( ) 2 γ against the square normalized wave

4 Square of growth rate γ 2
Square of wave number k * 2