Boundary Value Problems and Solutions

Abstract

In the previous chapters we have used the complete integrability of the stationary axisymmetric Einstein equations in vacuum to construct and to study rich classes of solutions which could describe the exterior gravitational .eld of stars and galaxies in thermodynamical equilibrium. In the present chapter we will use these methods to actually solve boundary value problems which are motivated by astrophysical models, in particular so-called dust disks.