  We continue a study by Adler and Ramazano\uglu (AR) of "black" holes as
modified by a scale invariant dark energy action. For the spherically symmetric
Schwarzschild-like case, (AR) found that there is no event horizon; hence
spacetime is not divided by the "black" hole into causally disconnected
regions. We review the formalism for locating trapped surfaces and apparent
horizons, and show that the modified "black" hole has no trapped surfaces. Thus
one suspects that it is "leaky", and that there will be a "black hole wind" of
particles streaming out from the location of the nominal horizon. This will
have astrophysical consequences, for example, the wind may feed and stabilize
star formation in the vicinity of the "black" hole. We initiate a study of the
stationary axially-symmetric rotating "black" hole as modified by a scale
invariant dark energy action, i.e, one that is Kerr-like. To set up the axial
case, we note that the conserving completion of the dark energy stress energy
tensor can be calculated algebraically by solving a $2 \times 2$ matrix
equation. Using Mathematica we calculate and simplify the modified system of
Einstein equations for the axial case in quasi-isotropic coordinates, and give
appropriate boundary conditions. Solution of these equations, which may require
developing a special purpose numerical program, is rendered tricky by a
residual general coordinate invariance of quasi-isotropic coordinates. This
leads to the interesting mathematical question of representing a positive
planar function as the gradient squared of a harmonic function.
