4.2. Kinetic and fluid descriptions
From the point of view of the evolution of largescale magnetic fields, the galaxy is globally neutral system of charged particles with typical rotation period of 3 × 10^{8} yrs. Two complementary descriptions of the plasma can then be adopted. The first possibility is to study the full system of kinetic equations (the VlasovLandau description [82, 83, 84] for the one particle distribution function). In the kinetic description the "observables" of the plasma dynamics are related to the various moments of the distribution function. In a complementary perspective, it is also possible to study directly the evolution equations of the various moments of the distribution function (charge and matter densities, momentum transfer etc.). The resulting description is an effective one since not all the moments of the distribution function can be kept. The necessity of a consistent truncation in the hierarchy of the various moments is usually called closure problem. MHD is an effective description which holding for
(4.7) 
where L and t are the typical length and time scales of the problem. The MHD approximation holds for typical length scales larger than the Debye scale and typical frequencies much smaller than the plasma frequency. In particular, the spectrum of plasma excitations obtained from the full kinetic description matches with the spectrum of MHD excitations but only at sufficiently small frequencies (typically of the order of the ionoacoustic waves) [85, 86].
If the plasma is weakly collisional and out of thermodynamical equilibrium, an approximation where the evolution equations are still tractable is given in terms of the oneparticle distribution function f_{i}(, , t) where the subscript denotes the given charge carrier (for instance electrons and ions). The oneparticle distribution obeys the VlasovLandau equation for each particle species of charge q_{i} and of mass m_{i}:
(4.8) 
The term appearing at the righthand side of Eq. (4.8) is the binary collision term. In a weakly coupled plasma, the longrange force is given by the Coulomb interaction, while the shortrange component arises thanks to binary collisions. In other words the electric and magnetic fields appearing in Eq. (4.8) are mean fields obeying mean Maxwell's equations:
(4.9)

where _{i} is the mean particle density. In the context of the kinetic approach the evolution equation should be solved selfconsistently with the Maxwell's equations. Clearly, in a system where the density of particles is small the mean field given by the distant particles is more important than the the force produced by the closest particles. In practice the Vlasovlandau system can be linearized around some equilibrium value of the oneparticle distribution function and specific examples will be discussed later on.
The oneparticle distribution function is not directly observable. The directly observable quantities are the the various moments of the oneparticle distribution, for instance, the particle density,
(4.13) 
and the related matter and charge densities for each particle species (i.e. _{m,i}(, t) = m_{i} n_{i}(, t) and _{q,i}(, t) = q_{i} n_{i}(, t)) or summed over the different species (i.e. _{m} = _{i} _{m,i} and _{q} = _{i} _{q,i}). However, the dynamical informations on the plasma evolution are not only encoded in the moment of order zero but also in the higher moments (the first, the second and even higher).
For some class of problems the kinetic approach is to be preferred. For instance the kinetic approach is mandatory for all the high frequency phenomena (like, for instance, equilibration of charge and current density fluctuations). As far as the lowfrequency phenomena are concerned one can imagine to obtain a reduced (fluidlike) description.