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Numerical results for the semi-classical stress-energy tensor outside thehorizon 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 theimplications for the black hole information paradox. Polynomial fits to thenumerical results for the 4D transverse stress are obtained forconformally-coupled spin 0 and spin 1 fields in the Hartle-Hawking and Unruhstates and. Analysis of the spin 0 Unruh state results clearly shows that theorigin of the Hawking radiation is not pair creation or tunneling very close tothe black hole horizon, but rather is a nonlocal process extending beyond r =3M . Arguments are presented that the black hole information paradox cannotplausibly be addressed by processes occurring on or very close to the horizonof a large black hole whose geometry is close to Schwarzschild.

Interpreting the semi-classical stress-energy tensor in a Schwarzschild background, implications for the information paradox