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-c onsistent three-dimensional solutions of the magnetohydrostatic (MHS) equat ions 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 constructi on of MHS solutions of this class with arbitrary photospheric boundary cond itions 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 a nd plasma temperature. The method therefore allows a better comparison of m odels with observations of solar coronal structures. We will demonstrate ho w the method works by giving an illustrative example.