  We report here on a new method for calculating the renormalized stress-energy
tensor (RSET) in black-hole (BH) spacetimes, which should also be applicable to
dynamical BHs and to spinning BHs. This new method only requires the spacetime
to admit a single symmetry. So far we developed three variants of the method,
aimed for stationary, spherically symmetric, or axially symmetric BHs. We used
this method to calculate the RSET of a minimally-coupled massless scalar field
in Schwarzschild and Reissner-Nordstrom backgrounds, for several quantum
states. We present here the results for the RSET in the Schwarzschild case in
Unruh state (the state describing BH evaporation). The RSET is type I at weak
field, and becomes type IV at $r\lesssim2.78M$. Then we use the RSET results to
explore violation of the weak and null Energy conditions. We find that both
conditions are violated all the way from $r\simeq4.9M$ to the horizon. We also
find that the averaged weak energy condition is violated by a class of
(unstable) circular timelike geodesics. Most remarkably, the circular null
geodesic at $r=3M$ violates the averaged null energy condition.
