Open access peer-reviewed chapter

Electrostatic Waves in Magnetized Electron-Positron Plasmas

By Ian Joseph Lazarus

Submitted: April 16th 2018Reviewed: August 16th 2018Published: December 17th 2018

DOI: 10.5772/intechopen.80958

Downloaded: 237

Abstract

The behavior of arbitrary amplitude linear and nonlinear electrostatic waves that propagate in a magnetized four component, two-temperature, electron-positron plasma is presented. The characteristics of the dispersive properties of the associated linear modes using both fluid and kinetic theory are examined. The fluid theory analysis of the electrostatic linear waves shows the existence of electron acoustic, upper hybrid, electron plasma and electron cyclotron branches. A kinetic theory analysis is then used to study the acoustic mode, in particular the effect of Landau damping, which for the parameter regime considered is due to the cooler species. Consequently, it is found that a large enough drift velocity is required to produce wave growth. Nonlinear electrostatic solitary waves (ESWs), similar to those found in the broadband electrostatic noise observed in various regions of the earth’s magnetosphere is further investigated. A set of nonlinear differential equations for the ESWs, which propagate obliquely to an external magnetic field is derived and numerically solved. The effect of various plasma parameters on the waves is explored and shows that as the electric driving force is increased, the electric field structure evolves from a sinusoidal wave to a spiky bipolar form. The results are relevant to both astrophysical environments and related laser-induced laboratory experiments.

Keywords

  • electrons
  • positrons
  • electrostatic waves
  • nonlinear waves

1. Introduction

Electron-positron plasmas play a significant role in the understanding of the early universe [1, 2], active galactic nuclei [3], gamma ray bursts (GRBs) [4], pulsar magnetospheres [5, 6] and the solar atmosphere [7]. These plasmas are also important in understanding extremely dense stars such as white dwarfs and pulsars, which are thought to be rotating neutron stars. The existence of these plasmas in neutron stars and in the pulsar magnetosphere is well documented [8]. The possibility for the co-existence of two types of cold and hot electron-positron populations in the pulsar magnetosphere has been suggested by [9] which was inspired by the pulsar model [10]. In their model, accelerated primary electrons moving on curved magnetic field lines emit curvature photons which produce electron-positron pairs. The secondary particles then produce curvature radiation, hence producing new electron-positron pairs, and so on. Therefore, both the electron and positron populations can be subdivided in two groups of distinct temperatures, one modeling the original plasma, and the second the higher-energy cascade-bred pairs. It is also known that in astrophysical and cosmic plasmas, a minority of cold electrons and heavy ions exist along with hot electron-positron pairs [11]. Hence, the formation of two temperature multispecies plasmas is possible due to the outflow of the electron-positron plasma from pulsars entering into an interstellar cold, low-density electron-ion plasma [12].

Investigations into electron-positron plasma behavior have focused primarily on the relativistic regime. It is however plausible that nonrelativistic astrophysical electron-positron plasmas may exist, given the effect of cooling by cyclotron emission [13]. The study of nonrelativistic astrophysical electron-positron plasmas therefore plays an important role in understanding wave fluctuations. Due to the equal charge to mass ratio for these oppositely charged species, only one frequency scale exists and due to this symmetry, there exists different physical phenomena to the conventional electron-ion plasmas. Further, the frequent instabilities that arise in space plasma and astrophysical environments (e.g., solar flames and auroras), involve the growth of electrostatic and electromagnetic waves which gives rise to a growing wave mode. In particular, the linear behavior of the electrostatic modes using fluid and kinetic theory approaches allows one to understand the effect of plasma parameters such as the propagation angle, cool to hot temperature ratios, density ratios and the magnetic field strength on the waves.

Investigations conducted have focused on modulational instabilities and wave localization [14], envelope solitons [15], multidimensional effects [16]. Large amplitude solitons and electrostatic nonlinear potential structures in electron-positron plasmas having equal hot and cold components of both species have been studied by a number of authors [17, 18, 19]. In one such study [20], using the two-fluid model with a single temperature they investigated linear and nonlinear longitudinal and transverse electrostatic and electromagnetic waves in a nonrelativistic electron-positron plasma in the absence and presence of an external magnetic field. They found that several of the modes present in electron-ion plasmas also existed in electron-positron plasmas, but in a modified form. Collective modes in nonrelativistic electron-positron plasmas using the kinetic approach was studied by [21]. The author found that the dispersion relations for the longitudinal modes in the electron-positron plasma for both unmagnetized and magnetized electron-positron plasmas were similar to the modes in one-component electron or electron-ion plasmas. Moreover, the hybrid resonances present in the former are not found in an electron-positron plasma.

The understanding of nonlinear wave structures which gives rise to electrostatic solitary wave (ESWs) in space is important since it is known that satellite measurements using high-time resolution equipment aboard spacecraft S3-3 [22], Viking [23], Geotail [24], Polar [25], and Fast [26] have indicated the presence of Broadband Electrostatic Noise (BEN) in the auroral magnetosphere at altitudes between 3000 km to 8000 km and beyond. These observations have shown the presence of electrostatic solitary waves (ESWs), which are characterized by their spiky bipolar pulses. Hence, the study of nonlinear wave behavior in electron-positron plasmas propagating at oblique angles to an ambient magnetic field is explored to understand electrostatic solitary waves in space. Specifically, the spiky nature of the electrostatic potential structures and the effects of the propagation angle, cold and hot drift velocities, cool to hot density and temperature ratios and Mach number on the ESWs are examined.

In this chapter a two-temperature magnetized four component electron-positron plasma model is used to study linear wave modes using both the fluid and kinetic approaches as well as the behavior of the nonlinear structures of these electrostatic solitary waves (ESWs) which plays an important role in space and astrophysical environments.

2. Linear waves in electron-positron plasmas: fluid theory approach

Let us consider a homogeneous magnetized, four component electron-positron plasma, consisting of cool electrons and cool positrons with equal temperatures and equilibrium densities denoted by Tcand n0c, respectively, and hot electrons and hot positrons with equal temperatures and equilibrium densities denoted by Thand n0h, respectively. The temperatures are expressed in energy units and wave propagation is taken in the x-direction at an angle θto the ambient magnetic field B0, which is assumed to be in the xzplane.

Assuming that the hot isothermal species are described by the Boltzmann distribution, their densities are, respectively

neh=n0hexpThE1

and

nph=n0hexpTh,E2

where neh(nph) is the density of the hot electrons (positrons) and ϕis the electrostatic potential.

Using Boltzmann distribution of hot electrons and positrons is justified provided they have sufficiently high temperatures, much greater than that of cooler species such that their thermal velocities parallel to the magnetic field exceed the phase velocity of the modes so that they are able to establish the Boltzmann distribution. The magnetic field effects on hot species are not felt since the perturbation wavelengths are shorter than their gyroradii such that both hot electrons and positrons follow essentially straight line orbits across the magnetic field direction.

The dynamics of cooler isothermal species are governed by fluid equations, namely the continuity equations,

njct+.njcvjc=0,E3

the equations of motion,

vjct+vjc.vjc=εjemϕ+εjemvjc×B0γTcnjcmnjc,E4

where εj= + 1(−1) for positrons (electrons), j=epfor the electrons (positrons). The system is closed by the Poisson equation

ε02ϕx2=enpcnec+nphneh.E5

In the above equations, njand vjare the number densities and fluid velocities respectively of the jthspecies. In order to derive the linear dispersion relation, equations (3)(5) are linearized. For perturbations varying as expikxωt, /tis replaced with and /xwith ik. Hence the perturbed densities for the electrons and positrons become

nec=n0cek2ϕmω2Ω2cos2θω4ω23k2vtc2+Ω2+3k2vtc2Ω2cos2θ.E6

and

npc=n0cek2ϕmω2Ω2cos2θω4ω23k2vtc2+Ω2+3k2vtc2Ω2cos2θ.E7

From equations (1) and (2), the perturbed densities for the hot species are given by,

neh=nohThE8

and

nph=nohTh.E9

Substituting equations (6)(9), into Poisson’s equation (5), the general dispersion relation for the two temperature electron-positron plasma is found to be

ω2ω2Ω23k2vtc2ω2Ω2cos2θk2vea21+12k2λDh2ω2Ω2cos2θ=0E10

where vea=n0c/n0h1/2vthis the acoustic speed of the electron-positron plasma, analogous in form to the electron acoustic speed in an electron-ion plasma [27]. The thermal velocity of the cool species is vtc=Tc/m1/2, Ωj=Ω=qjBo/mis the gyrofrequency of the electrons and positrons and λdh=ε0Th/n0he21/2is the Debye length of the hot species.

It is noted that the study of linear electrostatic waves using a simple fluid model cannot handle the possible Landau damping of the modes. Hence, Landau damping is not significant since phase velocities are far away from the thermal velocities of either the hot or cooler species, i.e., vthvϕvtcwith ThTc. The effects of the temperature variation on the acoustic mode in terms of Landau damping using kinetic theory are discussed in the next section.

For a single species electron-positron plasma, with temperature Tc, equation (10) reduces to,

ω4ω2Ω2+3k2vtc2+3k2vtc2Ω2cos2θ=0.E11

This is identical to the dispersion relation of [20] for their single temperature electron-positron model.

For wave frequencies much lower than the gyrofrequency and satisfying ωΩcosθ, the associated electron-acoustic (or positron-acoustic) mode is found to be,

ω2=k2vea2cos2θ1+12k2λDh2+3k2vtc2cos2θ.E12

Taking short wavelength limit (k2λDh21), the dispersion relation equation (10) reduces to,

ω4ω23k2vtc2+ωUH2+3k2vtc2+2ωpc2Ω2cos2θ=0,E13

where

ωUH2=Ω2+2ωpc2E14

is the upper hybrid frequency associated with the cooler species [20], with ωpc=noce2/ε0m1/2as the plasma frequency of the cooler species. If one solves equation (13) in the limit 3k2vtc2+ωUH2243k2vtc2Ω2cos2θ+2ωpc2Ω2cos2θ, one obtains for the upper hybrid mode,

ω+2=3k2vtc2+ωUH23k2vtc2+2ωpc2Ω2cos2θ3k2vtc2+ωUH2,E15

Taking the negative square root of equation (13) yields

ω2=3k2vtc2+2ωpc2Ω2cos2θ3k2vtc2+ωUH2,E16

In order to gain physical insight into the solution space of the dispersion relation, the two extreme limits of equation (10) will now be considered, viz. pure perpendicular and pure parallel propagations.

2.1 Case I: pure perpendicular propagation

Considering the pure perpendicular (θ=90o) limit, the general dispersion relation (10), reduces to:

ω4ω2Ω2+3k2vtc2+k2vea21+12k2λdh2=0.E17

Hence the normal mode frequencies are, ω=0, which is a nonpropagating mode, and

ω2=Ω2+3k2vtc2+k2vea21+12k2λdh2.E18

Taking the short wavelength limit (k2λdh21) of the above relationship, one obtains,

ω2=ωUH2+3k2vtc2.E19

showing that the behavior of the upper hybrid mode for the two temperature model is due to the cooler species, where ωUH2=Ωp2+2ωpc2.

Now taking the long wavelength limit (k2λdh21) of the dispersion relation for perpendicular propagation, equation (18) reduces to

ω2=Ω2+k23vtc2+vea2.E20

This is the cyclotron mode for the electron-positron plasma with contributions from both the thermal motion of the adiabatic cooler species and the acoustic motion due to the two species of different temperatures. To try and understand the physical implications, the above expression for the dispersion relation can be written as,

ω2=Ω2+k2vea21+3TcThn0hn0c.E21

For Tc/Th1, one requires n0hn0c, i.e., a plasma dominated by the hot species, in order for the second term in brackets to affect the dispersive properties of the wave.

2.2 Case II: pure parallel propagation

Considering the limit of parallel propagation (θ=0o), the general dispersion relation (10) reduces to,

ω4ω2Ω2+3k2vtc2+k2vea21+12k2λdh2+Ω23k2vtc2+k2vea21+12k2λdh2=0,E22

from which it can be shown

ω2=12Ω2+3k2vtc2+k2vea21+12k2λdh2±Ω23k2vtc2k2vea21+12k2λdh2.E23

There exist two possible solutions. Taking the positive sign of the relevant term in equation (23) as the first option yields,

ω+2=Ω2,E24

which is a constant frequency, nonpropagating cyclotron mode.

Now taking the negative sign of the term in equation (23) yields the normal mode frequency

ω2=3k2vtc2+k2vea21+12k2λdh2,E25

which may be written for k2λdh21as

ω2=k2vea21+3TcThn0hn0c,E26

which is identified fundamentally, as the electron-acoustic mode, with a correction term to its phase velocity due to the thermal motion of the cooler species.

In the limit k2λdh21, one obtains

ω2=3k2vtc2+2ωpc2E27

Equating equations (24) and (27) in the limit k2λdh21, the critical kvalue for which the two modes may couple is determined to be,

kλdcrit=Th3Tcn0cn01/2n0n0cR221/2.E28

A numerical analysis of the general dispersion relation can be performed focusing on the effects of the density and temperature ratios of the hot and cool electrons and positrons. If one normalizes the fluid speeds by the thermal velocity vth= Th/m1/2, the particle density by the total equilibrium plasma density n0=n0c+n0h, the temperatures by Th, the spatial length by λD=ε0Th/n0e21/2, and the time by ωp1=n0e2/ε0m1/2in equation (10), you get the normalized general dispersion relation,

ω'4ω'21R2+3k'2TcTh+k'2n0c'n0h'+12k'2+cos2θR23k'2TcTh+k'2n0c'n0h'+12k'2=0,E29

where ω'=ω/ωp, k'=kλD, n0h'=n0h/n0, n0c'=n0c/n0and R=ωp/Ωis a measure of the plasma densities and the strength of the magnetic field. A typical result can be seen in Figure 1 [28] for the normalized real frequency as a function of the normalized wavenumber showing the acoustic and cyclotron branches for a range of propagation angles.

Figure 1.

Normalized real frequency as a function of the normalized wavenumber showing the acoustic and cyclotron branches for various angles of propagation θ = 0o (solid), 9o (dotted), 22.5o (broken), 45o (dashddot) and 90o (longbroken). The fixed plasma parameters are R=0.333, Tc/Th=0.01 and n0c/n0h=0.11.

3. Linear waves in electron-positron plasmas: kinetic theory approach

In this section the kinetic theory approach is used to study the acoustic mode that was investigated in the previous section using fluid theory. The focus is on this mode since it is a micro-instability arising from resonances in velocity space. This instability is kinetic in nature and the growth rate of the wave is a function of the slope of the velocity distribution function. When the wave phase velocity along B0sees a negative slope of the velocity distribution f0/V<0, the particles on average will gain energy from the wave, consequently the wave losses energy and becomes damped, an effect known as Landau damping. The wave mode is hence subjected to Landau damping and wave enhancement. Therefore the focus in this section is primarily on the effect of the temperatures of the plasma species.

The same plasma model as in the previous section is considered, i.e., a four component magnetized electron-positron plasma, consisting of cool electrons and cool positrons with equal temperatures and equilibrium densities denoted by Tcand n0crespectively, and hot electrons and hot positrons with equal temperatures and equilibrium densities denoted by Thand n0h, respectively.

We begin by deriving the general dispersion relation where each species jhas an isotropic, drifting Maxwellian velocity distribution with temperatures Tjdrifting parallel to the magnetic field B0=B0ẑ, with drift velocities Voj.

Hence, the equilibrium velocity distribution for the electron and positron species is chosen to be,

fα0=nα02πvtj232expVx2+Vy2+VzVoj22vtj2,E30

The Vlasov equations are,

fαt+V.fα+qαmE+V×B.fαV=0,E31

and the equations of motion for the electrons and positrons is given by,

mdVdt=qαE+V×B,E32

where j=chfor the cool (hot) species and α=ec,pc,ehand phfor the cool electrons, cool positrons, hot electrons and hot positrons respectively, and vtj=Tj/m1/2is the thermal velocity of the jthspecies.

Following standard techniques for electron-ion plasmas [29], the general kinetic dispersion relation for the four component, two temperature electron-positron plasma is given by

k2+2λDc21+ωk.Voc2kvtcp=ZzpcΓpc+2λDh21+ωk.Voh2kvthp=ZzphΓph=0,E33

where λDc,h=ε0Th/n0c,he21/2is the Debye length for the cool (hot) species and zpjis the argument of the plasma dispersion function or Z-function [30] and is given by,

zpj=ωk.VojpΩj2kvtj,E34

where,

Γpj=eαjIpαj,E35

and

αj=k2vtj2Ωj2,E36

where Ipis the modified Bessel function of order p. The components of kparallel (perpendicular) to B0are given by k(k) respectively, while Vocand Vohare the drift velocities of the cool (hot) species, respectively.

3.1 Approximate solutions of the kinetic dispersion relation

The general dispersion relation (33) can be numerically solved without any approximations. However, to get some insight into the solutions, here, approximate expansions of the plasma dispersion function are used to obtain analytical expressions for the frequency and growth rate of the acoustic mode.

In proceeding, for the temperatures it is assumed that ThTc0. In addition low frequency modes satisfying ωΩare considered. The series expansion of the Z-function [30] is given by

Zz=iπez22z12z23+4z415forz1andE37
Zz=iπδez21z1+12z2+34z4+forz1.E38

where for z1, δ=0,Imz>01,Imz=02,Imz<0

Assuming the drift of the electrons and positrons to be weak (i.e., small Vocand Voh)[31] and ωΩ,

zpc=ωk.VocpΩ2kvtcpΩ2kvtcforp0E39

and

zph=ωk.VohpΩ2kvthpΩ2kvthforp0.E40

Then for the cool species,

p=ZzpcΓpcZωk.Voc2kvtcΓoc+p=1ZpΩ2kvtc+ZpΩ2kvtcΓpc.E41

From the definition of the Z-function, Zξ+Zξ=0, hence

p=ZzpcΓpcZzocΓoc.E42

Taking the cooler species to be stationary, Vocis therefore set to zero, allowing only the hot species to drift. Then,

zoc=ω2kvtc.E43

For modes satisfying ω/kvtc, one may assume zoc1, i.e., the wave phase speed along Bois much larger than the cool electron thermal speed. For instability (i.e., a growing wave with Imz>0), δis set equal to zero in equation (38). Hence using the series expansion equation (38), equation (41) becomes

p=ZzpcΓpc1zoc12zoc334zoc5Γoc.E44

Similarly, using the series expansion equation (37) (where ezoh21for zoh1), we have for the hot species,

p=ZzphΓphiπ2zoh+4zoh33Γoh.E45

It is noted that for relatively high temperature Th, the thermal velocity of the hot species is much larger than the wave phase velocity. Hence, for large Th, we have assumed that zoh1.

Substituting (44) and (45), λD, λDcand λDh, into the dispersion relation (33), whereas before λD=ε0Th/n0e21/2, gives

k2λD2+2n0cn0TcThiπzocezoc212zoc234zoc4+2n0hn01+iπzohΓoh=0.E46

For the cool species we have assumed αc=k2vtc2/Ω2=k2ρc21(where ρcis the gyroradius of the cool species), i.e., long wavelength fluctuations in comparison to ρc. Since in general for x1we can write Γpx=exIpxx/2p1/p!1x, hence we have Γoc1.

Second and higher order terms in zohare also neglected since we have assumed zoh1. Setting ω=ωr+and assuming γ/ωr1one may write

1ω21ωr212ωr.E47

Using the above manipulation the dispersion relation equation (46) becomes

k2λD2+2n0cn0TcThiπωr+2kvtcezoc2k2vtc2ωr212ωr3k4vtc4ωr412ωr2+2n0hn01+iπωr+k.Voh2kvthΓoh=0.E48

Taking the real part of equation (48) with the charge neutrality condition noc+noh=1, gives

ωr2=k2vea2cos2θ1+12k2λDh2+3k2vtc2cos2θ,E49

where cosθ=k/kand vea=n0c/n0h1/2vthis the acoustic speed of the electron-positron plasma. It is noted that equation (49) is consistent with the expression (12) obtained from fluid theory.

The approximate solution of the growth rate is determined by taking the imaginary part of equation (48), and hence solving for γ, one finds

γ=ωr4k3π81/2mTh3/2ThTc3/2ezoc2+n0hn0ck.Vohωr1Γoh1+6k2Tcmωr2.E50

We note that in equation (50), it is the cooler species that provides the Landau damping, i.e., the velocity distribution function sees a negative slope f0/V<0. It is also seen from equation (50) that for an unstable mode (γ>0), it is necessary that V0h>ωr/k, i.e., the drift velocity parallel to B0of the hot species has to be larger than the phase velocity to overcome the damping terms.

Normalizing the fluid speeds by the thermal velocity vth= Th/m1/2, the particle density by the total equilibrium plasma density n0=n0c+n0h, the temperatures by Th, the spatial length by λdj=ε0Tjn0je21/2, and the time by ωp1=n0e2ε0m1/2, one may write the normalized real frequency as,

ωr2=2n0ck2λd221n0c+k2λd2+3k2λd2TcTh,E51

and the approximate normalized growth rate as,

γr=ωr4k3λd3π81/21n0cn0ck.Vohωr1Γoh1+6k2TcThωr2,E52

For a fixed value of kλd, the real frequency increases with an increase in the cool to hot temperature ratio. This can be seen from the approximate analytical expression (51). Figure 2 displays the normalized growth rate as a function of the normalized wavenumber for varying cool to hot species temperature ratios Tc/Th. It is noted that as the Tc/Thdecreases, the growth rate increases, implying that the instability is more easily excited with lower temperature ratios. This may be explained as follows. As the temperature of the cooler species is increased, the associated Landau damping increases, resulting in a reduction of the overall growth rate. It is noted that a cutoff kλdvalue is reached beyond which the mode is damped.

Figure 2.

Normalized growth rate as a function of the normalized wavenumber. The fixed parameters are R=0.333, Voh=0.5, n0c=0.1 and θ=45o. The parameter labeling the curve is the cool to hot temperature ratio Tc/Th=0.005 (solid), 0.01 (dotted), and 0.02 (broken).

4. Nonlinear electrostatic solitary waves in electron-positron plasmas

The study of nonlinear effects in electron-positron plasmas is important since these plasmas exhibit different wave phenomena as compared to electron-ion plasmas. It is therefore important to understand the nonlinear structures, especially the solitary waves that exist in electron-positron plasmas. Satellite observations in the Earth’s magnetosphere have shown the existence of electrostatic solitary waves which forms part of broadband electrostatic noise (BEN) and electrostatic solitary waves (ESWs) in various regions of the Earth’s magnetosphere. The characteristic features of these ESWs are solitary bipolar pulses and consist of small scale, large amplitude parallel electric fields. These large amplitude spiky structures have been interpreted in terms of either solitons [32] or isolated electron holes in the phase space corresponding to positive electrostatic potential [33]. Given that electron-positron plasmas are increasingly observed in astrophysical environments, as well as in laboratory experiments [34], the above mentioned satellite observations also lead one to explore if such nonlinear structures are also possible in electron-positron plasmas. There is a distinct possibility that a pulsar magnetosphere can support coexistence of two types of cold and hot electron-positron populations [10, 35, 28]. In this section we investigate nonlinear electrostatic spiky structures in a magnetized four component two-temperature electron-positron plasma.

4.1 Basic equations

The model considered, as in the previous section is a homogeneous magnetized, four component, collisionless, electron-positron plasma, consisting of cool electrons (ec) and cool positrons (pc) with equal temperatures Tcand initial densities (nec0=npc0), and hot electrons (eh) and hot positrons (ph) with equal temperatures Thand densities (neh0=nph0). Wave propagation is taken in the x-direction at an angle θto the magnetic field B0, which is assumed to be in the x-zplane.

The continuity and momentum equations for the four species are given by

njt+njvjxx=0E53
vjxt+vjxvjxx+1njmpjx=εjemϕx+εjΩvjysinθE54
vjyt+vjxvjyx=εjΩvjzcosθεjΩvjxsinθE55
vjzt+vjxvjzx=εjΩvjycosθ,E56

where εj= + 1(−1) for positrons (electrons) and j=ec,pc,eh,phfor the cool electrons, cool positrons, hot electrons, and the hot positrons, respectively.

The density of the cool electrons (positrons) is nec(npc), and that of the hot electrons (positrons) is neh(nph).

The general equation of state for the four species is given by

pjt+vjxpjx+3pjvjxx=0,E57

The system is closed by the Poisson equation

ε02ϕx2=enpcnec+nphneh.E58

In the above equations, nj, vjand pjare the densities, fluid velocities and pressures, respectively, of the jthspecies. Ω=Ωe=Ωp=eB0/mis the cyclotron frequency. Here m= me= mpis the common mass of the electrons and the positrons. Adiabatic compression, γ=2+N/N=3, is assumed, where N=1 implies one degree of freedom.

Upon linearizing and combining equations (53)(58) and taking the limit vtcω/kvth, where vth=Th/m1/2and vtc=Tc/m1/2are the thermal velocities of the hot (cool) species, the dispersion relation equation for a magnetized two-temperature four component electron-positron plasma, where all species are governed by the fluid equations is,

ω4ω2Ω2+2ωs2+3k2vtc2+2ωs2Ω2cos2θ=0.E59

where ωpc,ph=n0c,he2/ε0m1/2are the plasma frequencies of the cool and hot species respectively and ωs=ωpc/1+2/3k2λDh21/2and λDh=ε0Th/nohe21/2.

Solving the above dispersion relation gives the cyclotron mode,

ω+2=Ω2+2ωs2+3k2vtc22ωs2Ω2cos2θΩ2+2ωs2+3k2vtc2E60

and the acoustic mode,

ω2=2ωs2Ω2cos2θΩ2+2ωs2+3k2vtc2,E61

4.2 Nonlinear analysis

In the nonlinear regime, a transformation to a stationary frame s=xVtΩ/Vis performed, and v,t,xand ϕare normalized with respect to vth, Ω1, ρ=vth/Ω, and Th/e, respectively. Vis the phase velocity of the wave. In equations (53)(57), /tis replaced by Ω/sand /xby Ω/V/s, and the diving electric field amplitude is defined as E=ψ/s, where ψ=/Th.

Integrating equation (53) and using the initial conditions nec0=n0and vecx=v0at s=0, yields the normalized velocity for the cool electrons in the x-direction.

vecx=neconecVv0+VE62

Similarly the cool positrons, hot electrons and hot positrons velocities are determined. Substituting these into the normalized form of equations (53)(57), gives the following set of nonlinear first-order differential equations for the cool electron species in the stationary frame.

ψs=EE63
Es=R2M2npcnnecn+nphnnehnE64
necns=necn3E+Msinθvecynnec0n02Mδc23TcThpecnnecnE65
vecyns=MnecnMδcn0nec0MMδcnecnnec0n0sinθ+veczncosθE66
veczns=n0nec0necnvecynMcosθMδcE67
pecns=3pecnnecn2E+Msinθvecynnec0n02Mδc23TcThpecnnecnE68

The set of differential equations for the cool positrons are given by,

npcns=npcn3Mδc2n0npc02EMsinθvpcynE69
vpcyns=MnpcnMδcn0npc0MMδcnpcnnpc0n0sinθvpczncosθE70
vpczns=n0npc0npcnvpcynMcosθMδcE71
ppcns=3ppcnnpcn2EMsinθvpcynnpc0n02Mδc23TcThppcnnpcnE72

Similar sets of differential equations can be derived for the hot electrons and hot positron species. The velocities are normalized with respect to the thermal velocity of the hot species vth=Th/m1/2and the densities with respect to the total density n0. The equilibrium density of the cool (hot) electrons is nec0neh0, and that of the cool (hot) positrons npc0nph0, with nec0+neh0=npc0+nph0=n0. R=ωp/Ω, where ωp=n0e2/ε0m1/2is the total plasma frequency, M=V/vthis the Mach number and δc,h=v0c,0h/vthis the normalized drift velocity of cool (hot) species at s=0. The system of nonlinear first-order differential equations can now be solved numerically using the Runge-Kutta (RK4) technique [36]. The initial values can be determined self consistently where the actual normalized electric fields are given by Enorm=1/Mψ/sand wave propagation is taken almost parallel to the ambient magnetic field B0.

Numerical results to investigate the effect of parameters such as the electric driving force E0, densities nec0and nph0, temperature ratio Tc/Th, Mach number M, drift velocities δc,hand propagation angle θon the wave can be explored. A typical numerical result is seen in Figure 3ad [37] showing the evolution of the system for various driving electric field amplitudes E0. It is seen that as E0increases, the electric field structure evolves from a sinusoidal wave to a sawtooth structure. For a higher E0value of 3.5, the potential structure has a spiky bipolar form showing that as the period of the wave increases and the frequency of the wave decreases.

Figure 3.

Numerical solution of the normalized electric field for the parameters M = 3.5, θ = 2o, R =10.0, δc = δh = 0.0, nec0/n0 = npc0/n0 =0.5, Tc/Th = 0.0, and E0 = (a) 0.05 [linear waveform], (b) 0.5 [sinusoidal waveform], (c) 1.5 [sawtooth waveform] and (d) 3.5 [bipolar waveform].

5. Conclusion

Linear and nonlinear electrostatic waves in a magnetized four component two-temperature electron-positron plasma have been investigated. In the linear analysis fluid and kinetic theory approaches are employed to describe the wave motion. The fluid theory approach focused on the wave dynamics of both the acoustic and cyclotron branches. Solutions of the dispersion relation from fluid theory yielded electron-acoustic, upper hybrid, electron plasma and electron cyclotron branches. Perpendicular and parallel wave propagation was examined showing its influence on the dispersive properties of the wave. The kinetic theory approach further examined Landau damping effects on the acoustic mode, analyzing the frequency and growth rate of the wave. The analysis shows that a large enough drift velocity (Voh) is required to produce wave growth. Both fluid and kinetic theory show excellent agreement for the real frequencies of the acoustic mode and solutions of the corresponding dispersion relation can be explored as a function of several plasma parameters. In the nonlinear analysis, the two-fluid model is used to derive a set of differential equations for the electrostatic solitary waves in a magnetized two-temperature electron-positron plasma. In particular, electrostatic solitary waves and their electric fields, similar to those found in the Broadband Electrostatic Noise are explored. For the onset of spiky ESWs, it is noted that as the wave speed increases, a larger driving electric field is required.

Acknowledgments

Thank you to Prof. Ramesh Bharuthram (University of the Western Cape, South Africa), Prof. Gurbax Lakhina and Prof. Satyavir Singh (Indian Institute of Geomagnetism, Navi Mumbai, India and Dr. Suleman Moolla (University of KwaZulu-Natal, Durban, South Africa) for your valuable contributions.

© 2018 The Author(s). Licensee IntechOpen. This chapter is distributed under the terms of the Creative Commons Attribution 3.0 License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

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Ian Joseph Lazarus (December 17th 2018). Electrostatic Waves in Magnetized Electron-Positron Plasmas, Charged Particles, Malek Maaza and Mahmoud Izerrouken, IntechOpen, DOI: 10.5772/intechopen.80958. Available from:

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