Lorentz ionization emerges due to the motion of atoms or ions in a strong m
agnetic field. We use the semiclassical approximation to calculate the prob
ability w(L) of Lorentz ionization. We also find the stabilization factor S
, which takes into account the reduction by the magnetic field of the proba
bility of ionization decay of the bound s state. We estimate the probabilit
ies w(L) in magnetic-cumulation experiments and in astrophysics. We also qu
alitatively examine the dynamics of the magnetic cumulation process with al
lowance for the conductivity of the shell. Finally, we discuss a paradox re
lated to the use of the quasistationary solution at the shell expansion sta
ge.(C) 1999 American Institute of Physics. [S1063-7761(99)00905-1].