Magnetosphere formation in the 3D kinetic approach by solar wind plasma flow characterized by shape of the particle distribution function. The new parameters of interaction and new spatial scalings

   The classic problem of the magnetosphere "outer" part formation by the
   solar wind plasma flow, including the forward effect, magnetotail
   formation, and the backward effect, dipolization, was considerd in the 3D
   large scale kinetic approximation via a self-consistent solutions of
   Vlasov/Maxwell equations. The "inner" magnetosphere is a specified source
   of distributed magnetization with magnetodipole and toroidal moments. The
   specified external flow of hot collisionless plasma, solar wind (SW,) is
   characterized by particle velocity distribution function (PDF) with
   different shapes. In the Chapman approach the SW flow is nonmagnetized
   plasma and formation of the magnetosphere is associated with the
   excitation of inductive electromagnetic fields (e.m.f) via the Cherenkov
   wide band resonance of magnetization source fields with flow particles in
   opacity and absorption mode. The magnetization source fields are screened
   by resistive and diamagnetic currents. We distinguish the resistive scale
   of anomalous screening associated with the process of particle
   acceleration by inductive electric fields, which provides dissipation and
   the effect of magnetic reconnection. We also get diamagnetic scale,
   associated with magnetic field effect on particles. The ratio of
   diamagnetic and resistive currents in the magnetosphere is characterized
   by the introduced G parameter which we call "the e.m. quality of the flow
   ". The value G depends on the shape of the PDF in the incoming SW plasma
   flow only. The e.m. quality value G determines the e.m. "space weather" in
   SW and magnetosphere transfer to dipolization state and vice-versa with a
   magnetotail. Note that acoustic Mach number characterizes the SW
   compressibility and the shock wave formation effect only. In the Dangey
   approach, the flow is magnetized by the "governing" magnetic (GM) field.
   The 3D kinetic approach is much more complicated, the plasma is MHD
   transparent in the wide band, that leads to e.m. radiation field formation
   in the magnetosphere distributed in the Alvenic cone due to the dispersion
   effects. The radiation free process of magnetotail formation and
   magnetosphere dipolization is associated with the effect of "narrow band
   ion-cyclotron anomalous screening of circular e.m.f". These e.m.f.
   constitute the magnetization source spectrum. New scales and dimensionless
   parameters were obtained for this process, they are defined via GM field
   (http://www.vniitf.ru/images/zst/2012/s3/3-13.pdf).