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Ions are Non-Thermal

Gurudas Mandalaand Prasanta Chatterjeeb,∗

aDepartment of ECE, East West University Mohakhali, Dhaka-1212, Bangladesh

bPlasma Physics Laboratory, Department of Physics, University of Malaya, Malaysia

On leave from the Department of Mathematics, Visva Bharati University, Santiniketan, India Reprint requests to G. M.; Fax: +880 28812336; E-mail: gdmandal@ewubd.edu

Z. Naturforsch.65a,85 – 90 (2010); received March 3, 2009

A four-component dusty plasma consisting of electrons, ions, and negatively as well as positively charged dust grains has been considered. Shock waves may exist in such a four-component dusty plasma. The basic characteristics of shock waves have been theoretically investigated by employing reductive perturbation technique (RPT). It is found that negative as well as positive shock potentials are present in such dusty plasma. The present results may be useful for understanding the existence of nonlinear potential structures that are observed in different regions of space (viz. cometary tails, lower and upper mesosphere, Jupiter’s magnetosphere, interstellar media, etc).

Key words:Dusty Plasma; Shock Waves; Non-Thermal; Dust Acoustic (DA) Wave.

1. Introduction

The nonlinear behaviour of charged dust particles has received much attention in the recent years because of its vital role in understanding of electrostatic density perturbations and nonlinear potential structures which are observed in different regions of space environ- ments, namely lower and upper mesosphere, cometary tails, planetary rings, planetary magnetosphere, inter- planetary space, interstellar media, etc. [1 – 4]. Most of the dusty plasma studies have been confined in con- sidering that the dust grains are negatively charged [5 – 11]. Very recent it has been found that there are some plasma systems, particularly in space plasma en- vironment, where positively charged dust grains are present and also play a significant role [2, 3, 12, 13].

There are three basic mechanisms by which the dust grains in the plasma system mentioned above can be positively charged [14]. These three mechanisms are the following: (i) photoemission in the presence of a flux of ultraviolet (UV) photons, (ii) thermionic emis- sion induced by radiative heating, and (iii) secondary emission of electrons from the surface of the dust grains.

Chow et al. [12] have shown theoretically that due to the size effect on secondary emission insulating dust grains with different sizes in space plasmas can have the opposite polarity (smaller ones being positive and larger ones being negative). This is mainly due to the

0932–0784 / 10 / 0100–0085 $ 06.00 c2010 Verlag der Zeitschrift f¨ur Naturforschung, T ¨ubingen·http://znaturforsch.com

fact that the excited secondary electrons have shorter (longer) distance to travel to reach the surface of the smaller (larger) dust grains [12].

There are also direct evidences for the existence of both positively and negatively charged dust parti- cles in different regions of space, viz. cometary tails [2, 3, 12], upper mesosphere [13], Jupiter’s magneto- sphere [15], etc. It has been suggested that the co- existence of positively and negatively charged dust are also present in laboratory plasmas [2, 3, 16]. On ba- sis of theoretical predictions and satellite observations, Mamun and Shukla [17] have considered a very sim- ple dusty plasma system, which assumes positively and negatively charged dust particles only, and have theo- retically investigated the properties of linear/nonlinear electrostatic waves that may propagate in such a dusty plasma system. This simple system is only valid if a complete depletion of background electrons and ions in the dusty plasma is considered. However, a com- plete depletion of background electrons and ions in most of the cases is not possible. Recently, Armina et al. [18] have considered a four-component dusty plasma containing positively and negatively charged dust and Boltzmann distributed electrons and ions.

They have investigated the possibility for the forma- tion of shock waves and also found the existence shock structures in this four-component dusty plasma. Re- cent observations [19, 20] show that the ion distribu- tion does not follow a Boltzmann distribution and in

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these cases the non-thermal distribution of ions is sug- gested.

In our present work, we considered a four-com- ponent unmagnetized dusty plasma system contain- ing Boltzmann distributed electrons, non-thermal dis- tributed ions, and also positively (smaller size) and negatively (larger size) charged dust grains.

The manuscript is organized as follows: The basic equations governing the dusty plasma system are pre- sented in Section 2. The nonlinear Burgers equation for the propagation of dust acoustic (DA) shock waves is derived in Section 3. The stationary shock wave solu- tion of the Burgers equation is analyzed in Section 4.

Finally, a brief discussion is presented in Section 5.

2. Governing Equations

We consider a one-dimensional (1D), unmagnetized collision less dusty plasma consisting of Boltzmann distributed electrons, non-thermal distributed ions, and positively and negatively charged dust grains. The non- linear dynamics of DA waves is governed by

n1

t + ∂

x(n1u1) =0, (1)

u1

t +u1u1

x =z1e m1·∂φ

xI2u1

x2, (2)

n2

t + ∂

x(n2u2) =0, (3)

u2

t +u2u2

x =−z2e m2·∂φ

xII2u2

x2, (4) ne−ni+z1n1−z2n2=0, (5) where n1(n2) is the negative (positive) dust num- ber density, u1(u2) is the negative (positive) dust fluid speed, z1(z2) is the number of electrons (pro- tons) residing on a negative (positive) dust particles, m1(m2) is the mass of negative (positive) dust parti- cle, −e is the electronic charge, φ is the wave po- tential, ηIII) is the viscosity coefficient of neg- ative (positive) dust fluid, x is the space variable, and t is the time variable. ne(ni) is the electron (ion) number density: ne =ne0e

eφ

kBTe, ni =ni0

1+ β1

kBTi

1

kBTi

2 e

eφ kBTe

, β1= 1+34α1α1, α1 is the non-thermal parameter that determines the num- ber of fast ions,Te(Ti) is the temperature of electrons (ions), andkB is the Boltzmann constant. In (5) we

have assumed the quasi-neutrality condition at equilib- rium. Now, in terms of normalized variables, namely N1=nn1

10,N2=nn2

20,U1=Cu1

1,U2=Cu2

1,ψ=k

BTi,T = tωpd,X=λx

D1IωpdλD22IIωpdλD2, where n10(n20)is equilibrium value ofn1(n2),C1=

z1kBTi

m1 , ωpd=

4πz12e2n10

m1 , andλD=

z1kBTi

4πz12e2n10. We can ex- press (1) – (5) as

N1

T + ∂

X(N1U1) =0, (6)

U1

T +U1U1

X =∂ψ

X12U1

X2, (7)

N2

T + ∂

X(N2U2) =0, (8)

U2

T +U2U2

X =αβ∂ψ

X22U2

X2, (9) N1= (1+µeµi)N2µeeσψ

i(1+β1ψ+β1ψ2)e−ψ, (10) where α = zz21, β = mm12, µe = z1nne010, µi = z1nni010, and σ=TTei.

3. Derivation of Burgers Equation

Now, we derive the Burgers equation from (6) – (10) by employing the reductive perturbation technique (RPT) and the stretch coordinates [21]ξ =ε1/2(X V0T), andτ=ε3/2T, whereεis a smallness parame- ter measuring the weakness of the nonlinearity andV0

is phase speed of the DA waves normalized byC1. We now express (6) – (10) in terms ofξ andτas

ε3/2N1

∂τ −V0ε1/2N1

∂ξ +ε1/2

∂ξ(N1U1) =0, (11) ε3/2U1

∂τ −V0ε1/2U1

∂ξ +ε1/2U1U1

∂ξ = ε1/2∂ψ

∂τ +ε3/2η102U1

∂ξ2,

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ε3/2N2

∂τ −V0ε1/2N2

∂ξ +ε1/2

∂ξ(N2U2) =0, (13) ε3/2U2

∂τ −V0ε1/2U2

∂ξ +ε1/2U2U2

∂ξ =

ε1/2αβ∂ψ

∂τ +ε3/2η202U2

∂ξ2,

(14)

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N1= (1+µeµi)N2µeeσψ

i(1+β1ψ+β1ψ2)e−ψ, (15) where η11/2η10 and η21/2η20 are assumed [17].

We can expand the variablesN1,U1,N2,U2, andψ in a power series ofεas

N1=1+εN1(1)2N1(2)+..., (16) U1=0+εU1(1)2U1(2)+..., (17) N2=1+εN2(1)2N2(2)+..., (18) U2=0+εU2(1)2U2(2)+..., (19)

ψ=0+εψ(1)2ψ(2)+... . (20)

Now, substituting (16) – (20) into (11) – (15) and taking the coefficient ofε3/2from (11) – (14) andεfrom (15) we have

N1(1)=U1(1)

V0 , (21)

U1(1)=ψ(1)

V0 , (22)

N2(1)=U2(1)

V0 , (23)

U2(1)= (αβ)ψ(1) V0

, (24)

N1(1)= (1+µeµi)N2(1)µeσψ(1)iβ1ψ(1). (25) Now, using (21) – (25) we get

N1(1)=ψ(1)

V02 , (26)

N2(1)= (αβ)ψ(1)

V02 , (27)

V02=1+αβ(1+µeµi)

σµeµiβ1 . (28) (28) is the linear dispersion relation for the DA waves propagating in our dusty plasma system. Similarly, substituting (16) – (20) into (11) – (15) and equating the coefficient ofε5/2from (11) – (14) andε2from (15) one obtains

N1(1)

∂τ −V0N1(2)

∂ξ +U1(2)

∂ξ +

∂ξ[N1(1)U1(1)] =0, (29)

U1(1)

∂τ −V0

U1(2)

∂ξ +U1(1)

U1(1)

∂ξ =∂ψ(2)

∂ξ +η102U1(1)

∂ξ2 , (30)

N2(1)

∂τ −V0

N2(2)

∂ξ +

U2(2)

∂ξ +

∂ξ[N2(1)U2(1)] =0, (31)

U2(1)

∂τ −V0

U2(2)

∂ξ +U2(1)

U2(1)

∂ξ =

αβ∂ψ(2)

∂ξ +η202U2(1)

∂ξ2 ,

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N1(2)= (1+µeµi)N2(2)µeσψ(2)

1

2µe(1)]2iβ1ψ(2)iβ1(1)]2. (33) Now, using (22), (24), and (26) – (28), and eliminating N1(2),N2(2),U1(2),U2(2), andψ(2), we finally obtain

∂ψ(1)

∂τ +Aψ(1)∂ψ(1)

∂ξ =C

2ψ(1)

∂ξ2 , (34) where the nonlinear coefficientA and the dissipation coefficientCare given by

A=3α2β2(1+µeµi)−3−V042µeiβ1) 2V0[1+αβ(1+µeµi)] , (35) C= η10+αβη20

2[1+αβ(1+µeµi)]. (36) (34) is known as Burgers equation which can describe the nonlinear propagation of DA waves in our four- component dusty plasma system.

4. Solution of Burgers Equation

The stationary solution of this Burgers equation is obtained by transforming the independent variablesξ andτtoζ=ξ−U0τandτ=τ, whereU0is a constant velocity normalized byC1, and imposing the appropri- ate boundary conditions, viz.ψ(1)0, ∂ψ(1)

ζ 0, at ζ ∞. Thus, one can express the stationary solution of the Burgers equation as

ψ(1)m(1)[1tanh(ζ/∆)], (37) where the amplitudeψm(1)(normalized bykBTi/e) and the width∆(normalized byλD) are given by

ψm(1)=U0

A, (38)

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Fig. 1.A=0 (β vs.µi) curves forα=0.01,σ=0.5,µe= 0.2 (solid curve),µe=0.3 (dotted curve),µe=0.4 (dashed curve).

Fig. 2. Positive shock potential profiles (ψvs.ζcurves) for α=0.01,σ=0.5,µi=0.5, µe=0.3,η10 =0.1,η20= 0.1β =400 (solid curve),β=500 (dotted curve),β=600 (dashed curve).

∆=2C

U0. (39)

It is observed from (37) – (39) that the amplitude (width) of the shock waves increases (decreases) asU0

increases. It is also clear from (35), (37), and (38) that shock potential profile is positive (negative) whenAis positive (negative). To find the different range of values ofβ andµifor which the positive and negative poten- tial profiles exist, we obtainA=0 (β vs. µi) curves.

TheA=0 (β vs.µi) curves are displayed in Figure 1.

From theseA=0 curves, we can have positive (nega- tive) shock potential profiles for the parameters whose values lie above (below) the curves.

Fig. 3. Negative shock potential profiles (ψvs.ζcurves) for α=0.01,σ=0.5,µi=0.5,µe=0.3,η10=0.1,η20=0.1 β=50 (solid curve),β=40 (dotted curve),β=30 (dashed curve).

Fig. 4. Positive amplitude profiles (ψmvs.µicurves) forα= 0.01,σ=0.5,β=400,η10=0.1,η20=0.1,µe=0.2 (solid curve),µe=0.3 (dotted curve),µe=0.4 (dashed curve).

Figure 2 and Figure 3 show how positive and neg- ative shock potentials vary with β. Figure 2 shows the positive shock potential profile, where the poten- tial decreases with the increase ofβ. Figure 3 shows the negative shock potential profile, where the poten- tial decreases with decrease ofβ. Figure 4 and Figure 5 show the positive (negative) amplitude (ψm) profiles of shock waves and how it varies withµe. Figure 4, for the positive amplitude profile shows that the amplitude of the shock waves increases asµeincreases. Figure 5, for the negative amplitude profile shows that the amplitude of shock waves decreases asµeincreases. Figure 6 and Figure 7 show how the width of shock waves varies (β =400 for Fig. 6 andβ =40 for Fig. 7) withµe. For both the values ofβ, the width (∆) of shock waves always decreases asµeincreases.

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Fig. 5. Negative amplitude profiles (ψm vs. µi curves) for α=0.01,σ=0.5,β =40,η10=0.1,η20=0.1,µe=0.2 (solid curve), µe=0.3 (dotted curve), µe=0.4 (dashed curve).

Fig. 6. Width profile (∆vs.µicurves) forα=0.01,σ=0.5, β=400,η10=0.1,η20=0.1,µe=0.2 (solid curve),µe= 0.3 (dotted curve),µe=0.4 (dashed curve).

5. Discussion

We have considered unmagnetized dusty plasma containing mobile positive and negative charged dust, Boltzmann electrons, and non-thermal distributed ions, and have theoretically investigated the basic features of the DA shock waves by employing the reductive per- turbation technique (RPT). It has been found in (35) that if we consider there is no positive dust grains in the plasma system, i. e.z2=0, henceα=0 thenAis always negative. It indicates only the existence of neg- ative shock potentials in the plasma system. We have then investigated the effect of coexistence of positive and negative dust grains, and we found that after cer- tain values ofα andβ(which corresponds to the pres-

Fig. 7. Width profile (∆vs.µicurves) forα=0.01,σ=0.5, β=40,η10=0.1,η20=0.1,µe=0.2 (solid curve),µe=0.3 (dotted curve),µe=0.4 (dashed curve).

ence of certain number of positive dust), one can have positive shock potential structures in the dusty plasma system. Armina et al. [18] found the similar result though they have considered the plasma system con- taining positive and negative dust grains, Boltzmann electrons and ions. The following features have been noticed in this theoretical investigation: (i) the ampli- tude of both the positive and negative shock poten- tial structures increases with increasing ofU0, (ii) the width of both the positive and negative shock potential structures decreases with increasing ofU0, (iii) the pos- itive and negative shock potentials are almost doubled when ion distribution is considered as non-thermal in- stead of Boltzmann ions [18], (iv) the potential of the positive shock structures decreases with increas- ing ofβ, (v) the potential of the negative shock struc- tures increases with increasing ofβ, (vi) the ampli- tude and the width of the DA shock waves are pos- itive for β =400 and both are decreasing with in- creasing of µe, (vii) the amplitude of the DA shock waves is negative for β =40 and is increasing with increasing ofµe, and (viii) the width of the DA shock waves is also decreasing forβ =40 with increasing ofµe.

It would be possible that the shock negative poten- tial may trap positively charged dust particles which can attract dust particles of opposite polarity to form larger sized dust or to be coagulated into extremely large sized neutral dust in cometary tails, upper meso- sphere, Jupiter’s magnetosphere or even in laboratory experiments.

The parameters chosen in our numerical calcula- tions are completely relevant to different regions of

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space, viz. cometary tails [2, 3, 12], mesosphere [13];

Jupiter’s magnetosphere [15], etc. In conclusion, we stress that our theoretical investigation and results may

also be applied to laboratory dusty plasma devices which will be able to produce a plasma containing pos- itive and negative dust grains.

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[2] D. A. Mendis and M. Rosenberg, Annu. Rev. Astron.

Astrophys.32, 419 (1994).

[3] M. Horanyi, Annu. Rev. Astron. Astrophys,34, 383 (1996).

[4] P. K. Shukla and A. A. Mamun, Introduction to Dust Plasma Physics, IoP Publishing Ltd., Bristol 2002.

[5] N. N. Rao, P. K. Shukla, and M. Y. Yu, Planet. Space Sci.38, 543 (1990).

[6] J. X. Ma and L. Liu, Phys. Plasmas4, 253 (1997).

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[11] J. K. Xue, Phys. Rev. E69, 016403 (2004).

[12] V. W. Chow., D. A. Mendis, and M. Rosenberg, J. Geo- phys. Res.98, 19065 (1993).

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Naesheim, E. Thrane, and T. Tønnesen, J. Geophys.

Res.101, 1039 (1996).

[14] V. E. Fortov, A. P. Nefedov, and O. S. Vaulina, J. Exp.

Theor. Phys.87, 1087 (1998).

[15] M. Horanyi, G. E. Morfill, and E. Grtin, Nature 363, l44 (1993).

[16] D. A. Mendis and M. Horanyi, in Cometary Plasma Processes, AGU Monograph61, 17 (1991).

[17] A. A. Mamun and P. K. Shukla, Geophys. Rev. Lett.29, 1870 (2002).

[18] R. Armina, A. A. Mamun, and S. M. K. Alam, Astro- phys. Space Sci.315, 243 (2008).

[19] R. Lundlin, A. Zakharov, R. Pelinenn, B. Hultqvist, H. Borg, E. M. Dubinin, S. Barabasj, N. Pissarenkon, H. Koskinen, and I. Liede, Nature341, 609 (1989).

[20] Y. Futaana, S. Machida, Y. Saito, A. Matsuoka, and H. Hayakawa, J. Geophys. Res.108, 151 (2003).

[21] H. Washimi and T. Taniuti, Phys. Rev. Lett.17, 996 (1966).

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