Speaker
Description
Through two exact solutions to the Einstein equation with sources, we show that general relativity allows two complementary descriptions for the microscopic state of BHs formed through gravitational collapse: (1) an ensemble of continuously contracting collapsars with close-to-implementing but never successfully implemented horizon in the Schwarzschild time definition, and (2) over-cross oscillatory solid-balls ergodically but unpredictably crossing the singularity in the Lemaitre time definition. The necessity of ensemble in the Schwarzschild time definition is due to the uncertainty of initial status, while the ergodicity of oscillations across the singularity is due to the unpredictability of motions over-cross the singularity. The complementarity of the two descriptions emerges naturally from the general coordinate invariance of GR rather than apriori assumptions required of any unknown quantum gravitation theory. The area-law formula of Bekenstein-Hawking entropy arises from the degeneracy of the quantised wave functional of the collapsing matter configurations. Our work provides a reconcilation for the contradiction between the statistic feature BH thermodynamics and the deterministic scenario of singularity theorems. It suggests that BHs maintain extended matter distributions of their progenitors rather than developing successfully implmented singularities or event horizons. This is a remarkable prediction testable through gravitational wave spectroscopy and multi-messenger astronomy.
| Research Area | Gravity: Geometric theory |
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