Under these conditions, assuming gravity and spacetime are quantized, a repulsive "force" arises from Heisenberg's uncertainty principle.
The accumulation of mass–energy inside the Planck star cannot collapse beyond this limit because it violates the uncertainty principle for spacetime itself.
[1] The key feature of this theoretical object is that this repulsion arises from the energy density, not the Planck length, and starts taking effect far earlier than might be expected.
This repulsive "force" is strong enough to stop the star's collapse well before a singularity is formed and, indeed, well before the Planck scale for distance: for a stellar mass black hole the Planck star would be of the order of 10−12 m - for a primordial black hole, the order of 10−16 m.[2]: whilst tiny, these scales are many orders of magnitude larger than the Planck length of 10−35 m. Then too, this allows adequate room for all the information captured inside a black hole to be encoded in the star, thus avoiding information loss.
Furthermore, the emission of Hawking radiation can be calculated to correspond to the timescale of gravitational effects on time,[clarification needed] such that the event horizon that "forms" a black hole evaporates as the rebound proceeds.