An Introduction to Plasma Physics and its Space Applications, Volume 2: Basic equations and applications by Luis Conde

Author:Luis Conde
Language: eng
Format: mobi, epub
ISBN: 9780750335430
Publisher: IOP Publishing
Published: 2020-08-24T16:00:00+00:00

1See equation volume 1, equation (2.2), box 2.2 and section 3.4.

2The equivalent time-independent averages were introduced in section 3.3 of volume 1.

3Strictly speaking, the Debye length expression (4.13) in volume 1 is derived for Maxwellian plasmas. This is not the general case, so in its place we can consider as an effective length scale for electric field shielding along which plasma quasineutrality is preserved.

a1 amu = 1.66 × 10−27 kg.

4We have and we also write . Equivalently gives and then .

5We make use of the internal energy of a monoatomic ideal, for molecules the factor 3/2 is replaced by where γ is the adiabatic index.

6Here the operation denotes the contraction of second order tensor with vector .

7For readers who are not familiar with this convected time derivative, it is introduced in appendix A.

8The distribution function normalization was different in sections 5.1 and 5.4 of volume 1, where , so , whereas here we use the definition (2.1) usual in kinetic theory and the integral over velocities gives the particle density (2.4).

9In the general case the thermal conductivity is also a tensor.

10The term ambipolar diffusion has a different meaning in astrophysics where it refers to the decoupling process of neutral atoms from the plasma during the initial stages of star formation.

11See sections 4.1 and 4.2 of reference [6].

12Since the ideal gas molecules have a Maxwell–Boltzmann energy distribution. Then, the equation of state is consistent with the assumption of a local Maxwellian electron population.

13See box 3.3, for the ideal gas law with Te constant recovered taking and the adiabatic transformation corresponds to with C constant.

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