Mass-Inflation in Dynamical Gravitational Collapse of a Charged Scalar-Field

We study the inner-structure of a charged black-hole which is formed from the gravitational collapse of a self-gravitating charged scalar-field. Starting with a regular spacetime, we follow the evolution through the formation of an apparent horizon, a Cauchy horizon and a final central singularity. We find a null, weak, mass-inflation singularity along the Cauchy horizon, which is a precursor of a strong, spacelike singularity along the r = 0 hypersurface. The no-hair theorem, introduced by Wheeler [1] in the early 1970s, states that the external field of a black-hole relaxes to a Kerr-Newman field characterized solely by the black-hole’s mass, charge and angular-momentum. This simple picture describing the exterior of a black-hole is in dramatic contrast with its interior. The singularity theorems of Penrose and Hawking [2] predicts the occurrence of inevitable spacetime singularities as a result of a gravitational collapse in which a black-hole forms. According to the weak cosmic censorship conjecture [3] these spacetime singularities are hidden beneath the black-hole’s event-horizon. However, these theorems tell us nothing about the nature of these spacetime singularities. In particular, the final outcome of a generic gravitational collapse is still an open question in general relativity. Until recently, our physical intuition regarding the nature of these inner singularities was largely based on the known static or stationary black-hole solutions: Schwarzschild (space-