Way down in the hole ... and up again

I argue that an approach which uses an appropriate admixture of both classical and semi-classical effects is essential for understanding the ultimate fate of gravitational collapse and the nature of black holes (BHs). I provide an example of a problem which pushes the boundaries of what is known in both the classical and semiclassical approaches: the evolution of the inner horizon of a BH. I show that solving this problem requires considering perturbations of both classical and semiclassical origins. In fact, it has been found that classical mass inflation might. be counteracted by a semiclassical tendency for the inner horizon to inflate outward.