Curvature properties of interior black hole metric
  A spacetime is a connected 4-dimensional semi-Riemannian manifold endowed with a metric $g$ with signature $(- + + +)$. The geometry of a spacetime is described by the metric tensor $g$ and the Ricci tensor $S$ of type $(0, 2)$ whereas the energy momentum tensor of type $(0,2)$ describes the physical contents of the spacetime. Einstein's field equations relate $g$, $S$ and the energy momentum tensor and describe the geometry and physical contents of the spacetime. By solving Einstein's field equations for empty spacetime (i.e. $S = 0$) for a non-static spacetime metric, one can obtain the interior black hole solution, known as the interior black hole spacetime which infers that a remarkable change occurs in the nature of the spacetime, namely, the external spatial radial and temporal coordinates exchange their characters to temporal and spatial coordinates, respectively, and hence the interior black hole spacetime is a non-static one as the metric coefficients are time dependent. For the sake of mathematical generalizations, in the literature, there are many rigorous geometric structures constructed by imposing the restrictions to the curvature tensor of the space involving first order and second order covariant differentials of the curvature tensor. Hence a natural question arises that which geometric structures are admitted by the interior black hole metric. The main aim of this paper is to provide the answer of this question so that the geometric structures admitting by such a metric can be interpreted physically. 
R. Deszcz, A.H. Hasmani, V.G. Khambholja and A.A. Shaikh
math.DG