  A technique is proposed for constructing three-dimensional solutions
comlplying with the self-consistent magnetohydrostatic (MHS) equations and with
observations along the line of sight of the magnetic field at the photosphere.
The technique is a generalization of a paper Rudenko, {\tt
arXiv:astro-ph/0004222} to a potential-field approximation. The solution of the
problem under consideration leans a representation of the magnetic field in
terms of a scalar function, with its subsequent harmonic expansion in terms of
a spherical functional basis that satisfies specified boundary conditions. A
numerical realization of the proposed method is expected to permit a real-time
modelling of three-dimensional magnetic field, temperature, pressure and
density distributions.
