STRINGS NEXT TO AND INSIDE BLACK-HOLES

The classical string equations of motion and constraints are solved ne ar the horizon and near the singularity of a Schwarzschild black hole. In a conformal gauge such that tau = 0 (tau = world sheet time coordi nate) corresponds to the horizon (r = 1) or to the black hole singular ity (r = 0), the string coordinates express in power series in tau nea r the horizon and in power series in tau(1/5) around r = 0. We compute the string invariant size and the string energy-momentum tenser. Near the horizon both are finite and analytic. Near the black hole singula rity, the string size, the string energy, and the transverse pressures (in the angular directions) tend to infinity as r(-1). To leading ord er near r = 0, the string behaves as two-dimensional radiation. These two spatial dimensions are describing the S-2 sphere in the Schwarzsch ild manifold.