Plasma Waves

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Plasma Waves Plasma Waves S.M.Lea January 2007 1 General considerations To consider the different possible normal modes of a plasma, we will usually begin by assuming that there is an equilibrium in which the plasma parameters such as density and magnetic field are uniform and constant in time. We will then look at small perturbations away from this equilibrium, and investigate the time and space dependence of those perturbations. The usual notation is to label the equilibrium quantities with a subscript 0, e.g. n0, and the pertrubed quantities with a subscript 1, eg n1. Then the assumption of small perturbations is n /n 1. When the perturbations are small, we can generally ignore j 1 0j ¿ squares and higher powers of these quantities, thus obtaining a set of linear equations for the unknowns. These linear equations may be Fourier transformed in both space and time, thus reducing the differential equations to a set of algebraic equations. Equivalently, we may assume that each perturbed quantity has the mathematical form n = n exp i~k ~x iωt (1) 1 ¢ ¡ where the real part is implicitly assumed. Th³is form descri´bes a wave. The amplitude n is in ~ general complex, allowing for a non•zero phase constant φ0. The vector k, called the wave vector, gives both the direction of propagation of the wave and the wavelength: k = 2π/λ; ω is the angular frequency. There is a relation between ω and ~k that is determined by the physical properties of the system. The function ω ~k is called the dispersion relation for the wave. ³ ´ A point of constant phase on the wave form moves so that dφ = ~k ~v ω = 0 dt ¢ Á ¡ where the wave phase velocity is ω ~vÁ = k^ (2) k The phase speed of a wave may (and often does) exceed the speed of light, since no information is carried at vÁ. Information is carried by a modulation of the wave, in either amplitude or frequency. For example, a wave pulse may have a Gaussian envelope. For any 1 physical quantity u, x2 /a2 ikx iωt u (x, t) = Ae¡ e ¡ Thus can be Fourier•transformed to yield a Gaussian in k space. ¡ A general disturbance of the system may be written as a superposition of plane waves. With x axis chosen along the direction of propagation for simplicity: ¡ + 1 1 ikx i!t u (x, t) = A (k) e ¡ dk p2π Z¡1 But ω is related to k through the dispersion relation: d! ω = ω (k) = ω + (k k ) + 0 ¡ 0 dk ¢ ¢ ¢ ¯k 0 ¯ where k is the wave number at which A (k) peaks. Then¯the integral becomes: 0 ¯ + 1 1 d! ikx i! 0t u (x, t) = A (k) e ¡ exp i (k k0) t dk p2π ¡ ¡ dk Z " ¯k 0 # ¡1 ¯ + ¯ 1 d! 1 ¯ d! = exp i k0 !0 t A (k) exp ik x t dk p2¼ dk ¡ ¡ dk " Ã ¯k 0 ! # Z " Ã ¯k0 !# ¯ ¡1 ¯ d! ¯ d! ¯ = exp i k ¯! t u x t; 0 ¯ 0 dk ¡ 0 ¡ dk " Ã ¯k 0 ! # Ã ¯k 0 ! ¯ ¯ Thus, apart from an overall ph¯ase factor, the disturbance p¯ ropagates at the group speed ¯ ¯ d! vg = (3) dk ¯k 0 ¯ Information travels at this group speed. ¯ ¯ Additional terms we have neglected in the exponent (involving the higher derivatives dn!=dkn ) give rise to pulse spreading and other factors generally referred to as dispersion. (More on this in Phys 704!) Hence the name "dispersion relation". Our goal will be to identify the different wave modes that occur in the plasma, and to find the dispersion relation ! ~k for each. If the frequency has an imaginary part, that indicates damping or growth o³f t´he wave. 2 Plasma oscillations In this wave we assume that the initial condition is a cold, uniform, unmagnetized plasma with n = n ; T 0 and ~v = 0: Then the equation of motion is: 0 ´ 0 @ mn ~v + ~v ~ ~v = en E~ 0 @t 1 1 ¢ r 1 ¡ 0 µ ³ ´ ¶ We ignore the second term on the left, because it involves a small quantity squared. Then we use the assumed wave form to obtain i!m~v = eE~ (4) ¡ 1 ¡ 2 Next the continuity equation gives @ (n + n ) + ~ (n + n ) ~v = 0 @t 0 1 r ¢ 0 1 1 @ n + n ~ ~v + ~ (n ~v ) = 0 @t 1 0r ¢ 1 r ¢ 1 1 ~ We used the facts that @n0=@t and n0 are zero. Again we ignore the last term because it involves the product of two small qurantities. Then: i!n + n ik~ ~v = 0 (5) ¡ 1 0 ¢ 1 Or, solving for n1; k~ ~v n = n ¢ 1 (6) 1 0 ! ~ Thus the density is not perturbed unless ~v1 has a component along k: This means that ~ transverse waves with ~v1 perpendicular to k do not perturb the plasma density. Finally we use Poissonzs equation, since this is a high•frequency wave: ~ ~ e e E = [n0 (n0 + n1)] = n1 r ¢ ¡ "0 ¡ ¡"0 This equation is already linear, and we get: ~ ~ e ik E = n1 (7) ¢ ¡ "0 Now we dot equation (4) with k~ and substitute in from equations (5) and (7). i!mk~ ~v = e~k E~ ¡ ¢ 1 ¡ ¢ !n e i!m 1 = e n ¡ n ¡ ¡ i" 1 0 µ 0 ¶ 2 !n1 e !m = n1 n0 "0 Now either n1 = 0 (not the result we want) or 2 2 n0e !p = (8) "0m The frequency of the disturbance is the plasma frequency !p: Notice that the result is independent of k: There is no phase speed or group speed: the wave is an oscillation that does not propagate. As we shall see, introduction of a non•zero temperature causes the wave to propagate. We can also see from equation (7) that the electric ®eld is out of phase with the density by ¼=2; while the velocity is in phase (equation 6). This oscillation is a fundamental mode of the plasma and has many ramifications. Our next step is to begin to investigate its importance. 3 3 Electromagnetic waves in an unmagnetized plasma To understand the importance of the plasma frequency a bit more, letzs look at the propagation of electromagnetic waves in the plasma. Maxwellzs equations are already linear. We have Poissonsz equation for E~ (7) and B~, i~k B~ = 0 (9) ¢ 1 Faradayzs Law i~k E~ = i!B~ (10) £ 1 and Amperezs law i~k B~ = ¹ ~j + i!" E~ (11) £ 0 0 The current in the plasma is due to the electron³and ion mo´tions: ~j = n e~v (n + n ) e~v 0 i ¡ 0 1 e For high frequency waves we may neglect the ion motion (~v 0) since the massive ions i ' do not respond rapidly enough as the driving force due to E~ changes. We also ignore the product of the two small quantities n1 and ve to get: ~j = n e~v (12) ¡ 0 e so that Amperezs law becomes: ik~ B~ = ¹ n e~v + i!" E~ (13) £ 1 0 ¡ 0 e 0 Finally we need the equation of motion for ³the electrons: ´ i!m~v = e E~ + ~v B~ (14) ¡ 1 ¡ e £ 1 which reduces to equation (4) when we ignore³the non•linear´term. Equation (6) shows that the density variations are zero for a transverse wave ~v perpendicular to ~k , and Poissonzs equation becomes k~ E~ = 0; which is consistent with ¢ t³he assumption of a tr´ansverse wave with ~v parallel to E~ (equation 14) . So let us look for transverse waves. Cross equation (13) with ~k to get: ik~ ~k B~ = ¹ n e~k ~v + i!" k~ E~ £ £ 1 0 ¡ 0 £ e 0 £ ³ ´ ³n e ´ ~k ~k B~ k2B~ = ¹ 0 ~k ~v ¹ !" !B~ ¢ 1 ¡ 1 ¡ 0 i £ e ¡ 0 0 1 where we used Far³adayzs l´aw. Further substitutions from equations (9) and (4) give: ~ 2 ~ n0e ~ eE 2 ~ k B1 = ¹0 k ¹0"0! B1 ¡ ¡ i £ Ã i!m ! ¡ e2 = ¹ n !B~ ¹ " !2B~ 0 0 !m ¡ 0 0 1 = ¹ " !2 !2 B~ (15) 0 0 p ¡ 1 ¡ ¢ 4 ~ ~ Again we argue that the solution B1 = 0 is uninteresting. The solution with non•zero B has 2 2 2 2 ! = k c + !p (16) 2 2 2 ! = k c + !p (17) Thus at high frquencies (! ! ) we have thqe usual vacuum relation ! = ck: À p 3 2.5 2 omega1.5 1 0.5 0 0.5 1 1.5ck 2 2.5 3 However, the wave number 2 2 ! !p k = ¡ q c becomes imaginary (k = i°) when ! < !p: The wave form becomes exp [i (i°) x i!t] = e °xei!t ¡ ¡ The wave does not propagate, and the disturbance damps as exp ( °x). The waves have a ¡ cut•off at ! = !p: An electromagnetic wave propagating at ! ! is able to excite plasma oscillations in · p the plasma, thus draining energy out of the wave and into the motion of plasma particles. Hence the wave damps. In the ionosphere with n 1012 m 3; the plasma frequency is » ¡ 12 3 19 2 1 (10 m¡ ) (1:6 10¡ C) fp = £ = 9: MHz 2¼ s (8:85 10 12 F/m) (9 10 31 kg) £ ¡ £ ¡ and waves at lower frequencies do not propagate through the ionosphere. This is an intrinsic limit on our ability to do radio astronomy from the Earthzs surface. If we do build a base on the moon, a radio observatory will quickly follow! The refractive index of the plasma is 2 c ck !p n = = = 1 2 (18) vÁ ! r ¡ ! and is less than one for all ! < : 1 5 1 0.8 n 0.6 0.4 0.2 0 1 2 omega 3 4 5 Snellsz law thus predicts the phenomenon of total external reflection when an EM wave of frequency ! < !p is incident on a plasma.
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