  We investigate a family of inhomogeneous and anisotropic gravitational fields
exhibiting a future singularity at a finite value of the proper time. The
studied spherically symmetric spacetimes are asymptotically
Friedmann-Robertson-Walker at spatial infinity and describe wormhole
configurations filled with two matter components: one inhomogeneous and
anisotropic fluid and another isotropic and homogeneously distributed fluid,
characterized by the supernegative equation of state \omega=p/\rho < -1. In
previously constructed wormholes, the notion of the phantom energy was used in
a more extended sense than in cosmology, where the phantom energy is considered
a homogeneously distributed fluid. Specifically, for some static wormhole
geometries the phantom matter was considered as an inhomogeneous and
anisotropic fluid, with radial and lateral pressures satisfying the relations
$p_{r}/\rho<-1$ and $p_{_l} \neq p_r$, respectively. In this paper we construct
phantom evolving wormhole models filled with an isotropic and homogeneous
component, described by a barotropic or viscous phantom energy, and ending in a
big rip singularity. In two of considered cases the equation of state parameter
is constrained to be less than -1, while in the third model the finite-time
future singularity may occur for $\omega<-1$, as well as for $-1 < \omega \leq
1$.
