The Green's function method for a special class of linear three-dimensional magnetohydrostatic equilibria.

We present the Green's function method for a special class of linear self-consistent three-dimensional solutions of the magnetohydrostatic (MHS) equations for which the current density is a combination of a linear force-free part and a part with non-fore e-free components. This allows the construction of MHS solutions of this class with arbitrary photospheric boundary conditions for B-z. These solutions can be used to extrapolate coronal magnetic fields from known longitudinal photospheric field data and provide a self-consistent description of magnetic field, plasma pressure, plasma density and plasma temperature. The method therefore allows a better comparison of models with observations of solar coronal structures. We will demonstrate how the method works by giving an illustrative example.