  A charged holostar is an exact solution of the Einstein field equations. Its
interior matter distribution rho = 1 / (8 pi r^2) is singularity free with an
overall string equation of state. It has a boundary membrane of tangential
pressure (but no mass-energy) situated roughly a Planck coordinate distance
outside of the outer horizon of the RN-solution with the same mass and charge.
  The geometric mass Mg = M + r0/2 of a charged holostar is always larger than
its charge. r0 is a Planck size correction to the gravitational mass M with r0
2 r_Pl. For a large holostar this condition is practically identical to the
classical condition M >= Q. Whereas RN solutions with M < Q are possible, a
charged holostar with Mg > Q doesn't exist.
  The total charge Q is derived by the proper integral over the interior charge
density, which is attributed to the charged massive particles. The interior
energy density splits into an electromagnetic and a "matter" contribution. Both
contributions are proportional to 1/r^2. The ratio of electro-magnetic to total
energy density rho_em / rho = 4 pi Q^2/A is constant throughout the whole
interior. It is related to the dimensionless ratio of the exterior conserved
quantities Q^2/A (or alternatively Q/M_g). An extremely charged holostar has a
surface area A = 4 pi Q^2, so that its interior energy density consists
entirely out of electromagnetic energy.
  A large holostar can be regarded as the classical analogue of a loop quantum
gravity (LQG) spin-network state. The Immirzi parameter is determined: g = s
/(pi \sqrt{3}), where s is the mean entropy per particle. g is larger by a
factor of ~4.8 than the LQG-result. An explanation for the discrepancy is
given.
