  Numerical results for the semi-classical stress-energy tensor outside the
horizon of a Schwarzschild black hole obtained in the 1980's and 1990's are re-
examined in order to better understand the origin of Hawking radiation and the
implications for the black hole information paradox. Polynomial fits to the
numerical results for the 4D transverse stress are obtained for
conformally-coupled spin 0 and spin 1 fields in the Hartle-Hawking and Unruh
states and. Analysis of the spin 0 Unruh state results clearly shows that the
origin of the Hawking radiation is not pair creation or tunneling very close to
the black hole horizon, but rather is a nonlocal process extending beyond r =
3M . Arguments are presented that the black hole information paradox cannot
plausibly be addressed by processes occurring on or very close to the horizon
of a large black hole whose geometry is close to Schwarzschild.
