  In order to understand the influence of magnetic fields on the propagation
properties of waves, as derived from different local helioseismology
techniques, forward modeling of waves is required. Such calculations need a
model in magnetohydrostatic equilibrium as initial atmosphere to propagate
oscillations through it. We provide a method to construct such a model in
equilibrium for a wide range of parameters to be used for simulations of
artificial helioseismologic data. The method combine the advantages of
self-similar solutions and current-distributed models. A set of models is
developed by numerical integration of magnetohydrostatic equations from the
sub-photospheric to chromospheric layers.
