  We describe the dynamics of a cosmological term in the spherically symmetric
case by an r-dependent second rank symmetric tensor \Lambda_{\mu\nu} invariant
under boosts in the radial direction. The cosmological tensor \Lambda_{\mu\nu}
represents the extension of the Einstein cosmological term \Lambda g_{\mu\nu}
which allows a cosmological constant be variable. This possibility is based on
the Petrov classification scheme and Einstein field equations in the
spherically symmetric case. The inflationary equation of state is satisfied by
the radial pressure p_r^{\Lambda}=-\rho^{\Lambda}. The tangential pressure is
calculated from the conservation equation \Lambda^{\mu}_{\nu;\mu}=0. The
solutions to the Einstein equations with cosmological term \Lambda_{\mu\nu}
describe several types of globally regular self-gravitating vacuum
configurations including vacuum nonsingular black holes. In this case the
global structure of space-time contains an infinite set of black and white
holes whose singularities are replaced with the value of cosmological constant
of the scale of symmetry restoration, at the background of asymptotically flat
or asymptotically de Sitter universes. We outline \Lambda white hole geometry
and estimate probability of quantum birth of baby universes inside a \Lambda
black hole. In the course of Hawking evaporation of a \Lambda black hole, a
second-order phase transition occurs, and globally regular configuration
evolves towards a self-gravitating particlelike structure at the background of
the Minkowski or de Sitter space.
