Appleton–Hartree equation

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] Further, regarding the derivation by Appleton, it was noted in the historical study by Gillmor that Wilhelm Altar (while working with Appleton) first calculated the dispersion relation in 1926.^[3]

Equation

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:

${\displaystyle n^{2}=\left({\frac {ck}{\omega }}\right)^{2}.}$ 

The full equation is typically given as follows:^[4]

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

or, alternatively, with damping term ${\displaystyle Z=0}$  and rearranging terms:^[5]

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

Definition of terms:

${\displaystyle n}$ : complex refractive index

${\displaystyle i={\sqrt {-1}}}$ : imaginary unit

${\displaystyle X={\frac {\omega _{0}^{2}}{\omega ^{2}}}}$ 

${\displaystyle Y={\frac {\omega _{H}}{\omega }}}$ 

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

${\displaystyle \nu }$ : electron collision frequency

${\displaystyle \omega =2\pi f}$ : angular frequency

${\displaystyle f}$ : ordinary frequency (cycles per second, or Hertz)

${\displaystyle \omega _{0}=2\pi f_{0}={\sqrt {\frac {Ne^{2}}{\epsilon _{0}m}}}}$ : electron plasma frequency

${\displaystyle \omega _{H}=2\pi f_{H}={\frac {B_{0}|e|}{m}}}$ : electron gyro frequency

${\displaystyle \epsilon _{0}}$ : permittivity of free space

${\displaystyle B_{0}}$ : ambient magnetic field strength

${\displaystyle e}$ : electron charge

${\displaystyle m}$ : electron mass

${\displaystyle \theta }$ : angle between the ambient magnetic field vector and the wave vector

Modes of propagation

The presence of the ${\displaystyle \pm }$  sign in the Appleton–Hartree equation gives two separate solutions for the refractive index.^[6] For propagation perpendicular to the magnetic field, i.e., ${\displaystyle \mathbf {k} \perp \mathbf {B} _{0}}$ , the '+' sign represents the "ordinary mode," and the '−' sign represents the "extraordinary mode." For propagation parallel to the magnetic field, i.e., ${\displaystyle \mathbf {k} \parallel \mathbf {B} _{0}}$ , 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.

${\displaystyle \mathbf {k} }$  is the vector of the propagation plane.

Reduced forms

Propagation in a collisionless plasma

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

${\displaystyle \nu \ll \omega }$ ,

we have

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

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

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

Quasi-longitudinal propagation in a collisionless plasma

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

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

See also

• Mary Taylor Slow
• Plasma (physics)
• Waves in plasmas

References

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 Electromagnetic Theory and Application. Pp 13–15. Kluwer Academic Publishers, 1991. Also available online, Google Books Scan
3. C. Stewart Gillmor (1982), Proc. Am. Phil. S, Volume 126. pp. 395
4. Helliwell, Robert (2006), Whistlers and Related Ionospheric Phenomena (2nd ed.), Mineola, NY: Dover, pp. 23–24
5. Hutchinson, I.H. (2005), Principles of Plasma Diagnostics (2nd ed.), New York, NY: Cambridge University Press, p. 109
6. Bittencourt, J.A. (2004), Fundamentals of Plasma Physics (3rd ed.), New York, NY: Springer-Verlag, pp. 419–429