The authors derive non-perturbative first and second laws for dynamical black holes, identifying entropy with the area of local marginally trapped surfaces rather than the global event horizon.
Dynamical Horizons and their Properties
7 Pith papers cite this work. Polarity classification is still indexing.
7
Pith papers citing it
abstract
A detailed description of how black holes grow in full, non-linear general relativity is presented. The starting point is the notion of dynamical horizons. Expressions of fluxes of energy and angular momentum carried by gravitational waves across these horizons are obtained. Fluxes are local and the energy flux is positive. Change in the horizon area is related to these fluxes. A notion of angular momentum and energy is associated with cross-sections of the horizon and balance equations, analogous to those obtained by Bondi and Sachs at null infinity, are derived. These in turn lead to generalizations of the first and second laws of black hole mechanics. The relation between dynamical horizons and their asymptotic states --the isolated horizons-- is discussed briefly. The framework has potential applications to numerical, mathematical, astrophysical and quantum general relativity.
citation-role summary
background 3
citation-polarity summary
roles
background 3polarities
background 3representative citing papers
Numerical study of cusp formation on horizons in head-on non-spinning black hole mergers, with analysis of mass and multipole behavior at the cusp and a proposed phenomenological model.
New general relativity does not admit physically meaningful non-trivial black holes distinct from those of the teleparallel equivalent of general relativity.
A new multi-scale hierarchical framework in GR uses matter horizons to extend perturbation theory beyond shell-crossing by gluing spacetimes with opposite orientation.
A novel exact solution describes a dynamical black hole dressed with a time-dependent scalar field and immersed in an axisymmetric time-dependent electromagnetic field, where time dependence may cloak curvature singularities.
A covariant zoom-in perturbation theory framework resolves geodesic breakdown via hierarchical matter horizons, producing an effective energy-momentum tensor whose backreaction explains flat galaxy rotation curves without dark matter.
In f(R) theories, the replica-method gravitational entropy computed on the apparent horizon matches the Hollands-Wald-Zhang dynamical black hole entropy and satisfies the first law, while the event horizon does not; this lets the generalized second law be reinterpreted as matter entanglement across
citing papers explorer
-
An essential building block for cosmological zoom-in perturbation theory
A new multi-scale hierarchical framework in GR uses matter horizons to extend perturbation theory beyond shell-crossing by gluing spacetimes with opposite orientation.
-
Cosmological zoom-in perturbation theory as a consistent beyond point-particle approximation framework
A covariant zoom-in perturbation theory framework resolves geodesic breakdown via hierarchical matter horizons, producing an effective energy-momentum tensor whose backreaction explains flat galaxy rotation curves without dark matter.