Book contents
- Frontmatter
- Contents
- Acknowledgements
- Introduction
- 1 Basic equations
- 2 Propagation in a cold plasma
- 3 Parallel propagation (weakly relativistic approximation)
- 4 Parallel propagation (non-relativistic approximation)
- 5 Quasi-longitudinal approximation
- 6 Quasi-electrostatic approximation
- 7 Growth and damping of the waves
- 8 Non-linear effects
- 9 Applications to the Earth's magnetosphere
- References
- Solutions to the problems
- Index
4 - Parallel propagation (non-relativistic approximation)
Published online by Cambridge University Press: 30 October 2009
- Frontmatter
- Contents
- Acknowledgements
- Introduction
- 1 Basic equations
- 2 Propagation in a cold plasma
- 3 Parallel propagation (weakly relativistic approximation)
- 4 Parallel propagation (non-relativistic approximation)
- 5 Quasi-longitudinal approximation
- 6 Quasi-electrostatic approximation
- 7 Growth and damping of the waves
- 8 Non-linear effects
- 9 Applications to the Earth's magnetosphere
- References
- Solutions to the problems
- Index
Summary
The general dispersion equation for whistler-mode propagation, instability or damping in a non-relativistic plasma with the electron distribution function in the form (1.90) has already been derived in Section 3.1 (see equation (3.20)). Assuming, as in Sections 1.2 and 3.2, that whistler-mode growth or damping does not influence wave propagation we can simplify equation (3.20) to:
where N, ω and Y hereafter in this chapter are assumed to be real, the argument of the Z function is ξ1 = ξ = (1 Y)/Nῶ∥, ῶ∥ = w∥/c (cf. similar assumptions in Section 3.2),
(cf. the definition of the Z function by equation (1.21)), and Ae = (j + 1) w⊥2/w∥2 (when deriving (4.1) we have generalized equation (3.20) for arbitrary integer j).
As follows from the analysis of Chapter 3, the non-relativistic approximation and, in particular, equation (4.1) is valid in a relatively dense plasma when ν ≫ 1 and N2 ≫ 1, in general. Hence, the second term ‘1’ in equation (4.1) will either be neglected altogether or taken into account when calculating the perturbation of N2 due to non-zero ν− 1 (cf. equation (3.34)).
Although equation (4.1) is much simpler than the corresponding weakly relativistic dispersion equation (cf. equation (3.10)), it still has no analytical solution in general.
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- Whistler-mode Waves in a Hot Plasma , pp. 76 - 93Publisher: Cambridge University PressPrint publication year: 1993