  Einstein equations projected on black-hole horizons give rise to the
equations of motion of a viscous fluid. This suggests a way to understand the
microscopic degrees of freedom on the black-hole horizon by focusing on the
physics of this fluid. In this talk, we shall approach this problem by building
a crude microscopic model for the Horizon-fluid(HF) corresponding to
asymptotically flat black-holes in 3+1 dimensions. The symmetry requirement for
our model is that it should incorporate the S1 diffeo-symmetry on the
black-hole horizon. The second constraint comes from the demand that the
correct value of the Coefficient of the Bulk Viscosity of the HF can be deduced
from the model. Both these requirements can be satisfied by an adoption of the
eight vertex Baxter model on a S2 surface. We show that the adiabatic entropy
quantisation proposed by Bekenstein also follows from this model. Finally, we
argue the results obtained so far suggest that a perturbed black-hole can be
described by a CFT perturbed by relevant operators and discuss the physical
implications.

General Relativity and Quantum Cosmology;Statistical Mechanics;High Energy Physics - Theory