Appleton–Hartree equation

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The Appleton–Hartree equation, sometimes also referred to as the Appleton–Lassen equation is a mathematical expression that describes the refractive index for electromagnetic wave propagation in a cold magnetized plasma. The Appleton–Hartree equation was developed independently by several different scientists, including Edward Victor Appleton, Douglas Hartree and German radio physicist H. K. Lassen.[1] Lassen's work, completed two years prior to Appleton and five years prior to Hartree, included a more thorough treatment of collisional plasma; but, published only in German, it has not been widely read in the English speaking world of radio physics.[2]

Equation[edit]

The dispersion relation can be written as an expression for the frequency (squared), but it is also common to write it as an expression for the index of refraction n^2 = \left(\frac{ck}{\omega}\right)^2 .

Full Equation[edit]

The equation is typically given as follows:[3]

n^2 = 1 - \frac{X}{1 - iZ - \frac{\frac{1}{2}Y^2\sin^2\theta}{1 - X - iZ} \pm \frac{1}{1 - X - iZ}\left(\frac{1}{4}Y^4\sin^4\theta + Y^2\cos^2\theta\left(1 - X - iZ\right)^2\right)^{1/2}}

or, alternatively, with damping term Z = 0 and rearranging terms:[4]

n^2 = 1 - \frac{X\left(1-X\right)}{1 - X - {\frac{1}{2}Y^2\sin^2\theta} \pm \left(\left(\frac{1}{2}Y^2\sin^2\theta\right)^2 + \left(1-X\right)^2Y^2\cos^2\theta\right)^{1/2}}

Definition of Terms[edit]

n = complex refractive index

i = \sqrt{-1}

X = \frac{\omega_0^2}{\omega^2}

Y = \frac{\omega_H}{\omega}

Z = \frac{\nu}{\omega}

\nu = electron collision frequency

\omega = 2\pi f (radial frequency)

f = wave frequency (cycles per second, or Hertz)

\omega_0 = 2\pi f_0 = \sqrt{\frac{Ne^2}{\epsilon_0 m}} = electron plasma frequency

\omega_H = 2\pi f_H = \frac{B_0 |e|}{m} = electron gyro frequency

\epsilon_0 = permittivity of free space

B_0 = ambient magnetic field strength

e = electron charge

m = electron mass

\theta = angle between the ambient magnetic field vector and the wave vector

Modes of propagation[edit]

The presence of the \pm sign in the Appleton–Hartree equation gives two separate solutions for the refractive index.[5] For propagation perpendicular to the magnetic field, i.e., \bold k\perp \bold B_0, the '+' sign represents the "ordinary mode," and the '−' sign represents the "extraordinary mode." For propagation parallel to the magnetic field, i.e., \bold k\parallel \bold B_0, the '+' sign represents a left-hand circularly polarized mode, and the '− sign represents a right-hand circularly polarized mode. See the article on electromagnetic electron waves for more detail.

\bold k is the vector of the propagation plane.

Reduced Forms[edit]

Propagation in a collisionless plasma[edit]

If the electron collision frequency \nu is negligible compared to the wave frequency of interest \omega, the plasma can be said to be "collisionless." That is, given the condition

\nu \ll \omega,

we have

Z = \frac{\nu}{\omega} \ll 1,

so we can neglect the Z terms in the equation. The Appleton–Hartree equation for a cold, collisionless plasma is therefore,

n^2 = 1 - \frac{X}{1 - \frac{\frac{1}{2}Y^2\sin^2\theta}{1 - X} \pm \frac{1}{1 - X}\left(\frac{1}{4}Y^4\sin^4\theta + Y^2\cos^2\theta\left(1 - X\right)^2\right)^{1/2}}

Quasi-Longitudinal Propagation in a Collisionless Plasma[edit]

If we further assume that the wave propagation is primarily in the direction of the magnetic field, i.e., \theta \approx 0, we can neglect the Y^4\sin^4\theta term above. Thus, for quasi-longitudinal propagation in a cold, collisionless plasma, the Appleton–Hartree equation becomes,

n^2 = 1 - \frac{X}{1 - \frac{\frac{1}{2}Y^2\sin^2\theta}{1 - X} \pm Y\cos\theta}

References[edit]

Citations and notes
  1. ^ Lassen, H., I. Zeitschrift für Hochfrequenztechnik, 1926. Volume 28, pp. 109–113
  2. ^ C. Altman, K. Suchy. Reciprocity, Spatial Mapping and Time Reversal in Electromagnetics – Developments in Eelctromagnetic Theory and Application. Pp 13–15. Kluwer Academic Publishers, 1991. Also available online, Google Books Scan
  3. ^ Helliwell, Robert (2006), Whistlers and Related Ionospheric Phenomena (2nd ed.), Mineola, NY: Dover, pp. 23–24 
  4. ^ Hutchinson, I.H. (2005), Principles of Plasma Diagnostics (2nd ed.), New York, NY: Cambridge University Press, p. 109 
  5. ^ Bittencourt, J.A. (2004), Fundamentals of Plasma Physics (3rd ed.), New York, NY: Springer-Verlag, pp. 419–429 

See also[edit]