  We study how the evaporation rate of spherically symmetric black holes is
affected through the extraction of radiation close to the horizon. We adopt a
model of extraction that involves a perfectly absorptive screen placed close to
the horizon and show that the evaporation rate can be changed depending on how
close to the horizon the screen is placed. We apply our results to show that
the scrambling time defined by the Hayden-Preskill decoding criterion, which is
derived in Pennington's work (arXiv:1905.08255) through entanglement wedge
reconstruction is modified. The modifications appear as logarithmic corrections
to Pennington's time scale which depend on where the absorptive screen is
placed. By fixing the proper distance between the horizon and screen we show
that for small AdS black holes the leading order term in the scrambling time is
consistent with Pennington's scrambling time. However, for large AdS black
holes the leading order Log contains the Bekenstein-Hawking entropy of a cell
of characteristic length equal to the AdS radius rather than the entropy of the
full horizon. Furthermore, using the correspondence between the radial null
energy condition (NEC) and the holographic c-theorem, we argue that the screen
cannot be arbitrarily close to the horizon. This leads to a holographic
argument that black hole mining using a screen cannot significantly alter the
lifetime of a black hole.
