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5.4. Charge and current density fluctuations

As a simple application of kinetic techniques, it is useful to understand which magnetic field can be obtained from an initial inhomogeneous distribution of charge and current density fluctuations.

Consider then the system of Eqs. (5.38) under the assumption that, initially, electric and magnetic fields vanish:

Equation 5.68 (5.68)

Using Eqs. (5.36)-(5.38) the induced magnetic fields can be obtained.. This problem is discussed, in greater detail, in [134].

Subtracting Eqs. (5.36) and (5.37), and defining

Equation 5.69 (5.69)

the Vlasov-Landau system can be written as

Equation 5.70-5.74 (5.70)





where gvector{k}(vector{p}) is the initial profile of the distribution function and where tilde{nu} is the typical collision frequency. The subscripts vector{k} omega denote the Fourier transform with respect to space and the Laplace transform with respect to time of the corresponding quantity.

After enforcing the Gauss constraint at the initial time, the electric field can be separated in its polarizations parallel and transverse to the direction of propagation of the fluctuation. The transverse current provides a source for the evolution of transverse electric field fluctuations

Equation 5.75 (5.75)

whereas the charge fluctuations provide a source for the evolution of longitudinal electric field fluctuations

Equation 5.76 (5.76)

In Eqs. (5.75) and (5.76) the longitudinal and transverse part of the electric field fluctuations have been defined:

Equation 5.77 (5.77)

The solution of Eq. (5.70) is given by

Equation 5.78 (5.78)

where we used that partialf0 / partial vector{p} ident vector{v} partialf0 / partialp. The longitudinal and transverse components of the electric fluctuations can be obtained by inserting Eq. (5.78) into Eqs. (5.75)-(5.76)

Equation 5.79-5.80 (5.79)


where epsilon|| and epsilonperp are, respectively, the longitudinal and transverse part of the polarization tensor

Equation 5.81-5.82 (5.81)


Now, the general expression for the generated magnetic field is

Equation 5.83 (5.83)

The space-time evolution of the magnetic fluctuations can be determined by performing the inverse Laplace and Fourier transforms:

Equation 5.84 (5.84)

In order to perform this integral, the explicit relations for the polarization tensors should be given. They depend on the equilibrium distribution function f0(p), which we take to be the expression given in Eq. (5.34) (21)

Then we have for transverse polarization

Equation 5.85 (5.85)

and for the longitudinal polarization:

Equation 5.86 (5.86)

Consider now the case of very small momenta k << omega and omega << tilde{nu}, relevant for long-ranged magnetic fields. Then the computation of the integral (5.84) in the large time limit and with the use of explicit form of the transverse polarization tensor in (5.85) gives (22):

Equation 5.87 (5.87)

where sigma is the plasma conductivity in the relaxation time approximation,

Equation 5.88 (5.88)

and initial electric current is given by

Equation 5.89 (5.89)

The obtained results assumed that the linearization of the Vlasov equation is consistent with the physical assumptions of our problem. This is indeed the case. In order to safely linearize the Vlasov equation we have to make sure that the perturbed distribution function of the charge fluctuations is always smaller than the first order of the perturbative expansion (given by the distribution of Eq. 5.34). In other words we have to make sure that

Equation 5.90 (5.90)

These conditions imply that

Equation 5.91 (5.91)

If the relativistic plasma frequency is defined,

Equation 5.92 (5.92)

the condition expressed by Eq. (5.91) can be restated, for modes k leq omegap, as |vector{E}vector{k},omega|2 < nqT (where we essentially took the square modulus of Eq. (5.91)). This last inequality expresses the fact that the energy density associated with the gauge field fluctuations should always be smaller than the critical energy density stored in radiation. The linear treatment of the Vlasov equation is certainly accurate provided the typical modes of the the field are smaller than the plasma frequency and provided the energy density in electric and magnetic fields is smaller than T4, i.e. the energy density stored in the radiation background.

21 Notice that most of our considerations can be easily extended to the case of a Bose-Einstein or Fermi-Dirac distribution. What is important, in our context, is the analytical structure of the polarization tensors and this is the same for different distributions [125]. Back.

22 For small k, the equation omega2 epsilonperp(k, omega) - k2 = 0 defining the poles of the inverse Laplace transform implies omega ~ i k2 / sigma. Back.

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