  General Relativity predicts the existence of black-holes. Access to the
complete space-time manifold is required to describe the black-hole. This
feature necessitates that black-hole dynamics is specified by future or
teleological boundary condition. Here we demonstrate that the statistical
mechanical description of black-holes, the raison d'etre behind the existence
of black-hole thermodynamics, requires teleological boundary condition. Within
the fluid-gravity paradigm --- Einstein's equations when projected on
space-time horizons resemble Navier-Stokes equation of a fluid --- we show that
the specific heat and the coefficient of bulk viscosity of the horizon-fluid
are negative only if the teleological boundary condition is taken into account.
We argue that in a quantum theory of gravity, the future boundary condition
plays a crucial role. We briefly discuss the possible implications of this at
late stages of black-hole evaporation.
