  The lower solar atmosphere is an intrinsically multi-component and
collisional environment with electron and proton collision frequencies in the
range $10^{8}-10^{10}$ Hz, which may be considerably higher than the
gyro-frequencies for both species. We aim to provide a reliable quantitative
set of data for collision frequencies, magnetization, viscosity, and thermal
conductivity for the most important species in the lower solar atmosphere.
Having such data at hand is essential for any modeling that is aimed at
describing realistic properties of the considered environment.
  We describe the altitude dependence of the parameters and the different
physics of collisions between charged species, and between charged and neutrals
species. Regions of dominance of each type of collisions are clearly
identified. We determine the layers within which either electrons or ions or
both are unmagnetized. Protons are shown to be un-magnetized in the lower
atmosphere in a layer that is at least 1000 km thick even for a kilo-Gauss
magnetic field that decreases exponentially with altitude. In these layers the
dynamics of charged species cannot be affected by the magnetic field, and this
fact is used in our modeling. Viscosity and thermal conductivity coefficients
are calculated for layers where ions are unmagnetized. We compare viscosity and
friction and determine the regions of dominance of each of the phenomena.
  We provide the most reliable quantitative values for most important
parameters in the lower solar atmosphere to be used in analytical modeling and
numerical simulations of various phenomena such as waves, transport and
magnetization of particles, and the triggering mechanism of coronal mass
ejections.
