2010/04/04 by Jonathan Ziprick, G. Kunstatter, Gabor Kunstatter · 1 citation
Mathematics · Physics and Astronomy · #Apparent horizon #Black Holes and Theoretical Physics #Classical mechanics #Cosmology and Gravitation Theories #Energy condition #Event horizon #General relativity #Geometry #Gravitational collapse #Mathematical physics #Mathematics #Naked singularity #Negative energy #Noncommutative and Quantum Gravity Theories #Physics #Quantum #Quantum gravity #Quantum mechanics #Singularity #Spacetime #gr-qc
paper · pdf · doi:10.1103/physrevd.82.044031
published as Phys.Rev.D82:044031,2010
arxiv created 2010/04/04 · openalex publication_date 2010/08/13 · arxiv updated 2015/03/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
A phenomenological framework is presented for incorporating quantum gravity motivated corrections into the dynamics of spherically symmetric collapse. The effective equations are derived from a variational principle that guarantees energy conservation and the existence of a Birkhoff theorem. The gravitational potential can be chosen as a function of the areal radius to yield specific nonsingular static spherically symmetric solutions that generically have two horizons. For a specific choice of potential, the effective stress energy tensor violates only the dominant energy condition. The violations are maximum near the inner horizon and die off rapidly. A numerical study of the quantum corrected collapse of a spherically symmetric scalar field in this case reveals that the modified gravitational potential prevents the formation of a central singularity and ultimately yields a static, mostly vacuum, spacetime with two horizons. The matter ``piles up'' on the inner horizon giving rise to mass inflation at late times. The Cauchy horizon is transformed into a null, weak singularity, but in contrast to Einstein gravity, the absence of a central singularity renders this null singularity stable.