  For any configuration of a static plane-symmetric distribution of matter
along space-time, there are coordinates where the metric can be put explicitly
as a functional of the energy density and pressures. It satisfies Einstein
equations as far as we require the conservation of the energy-momentum tensor,
which is the single ODE for self-gravitating hydrostatic equilibrium. As a
direct application, a general solution is given when the pressures are linearly
related to the energy density, recovering, as special cases, most of known
solutions of static plane-symmetric Einstein equations.
