Traditional black holes (Schwarzschild black holes) are solutions to the Einstein field equations under spherically symmetric and static conditions, with their physical effects mainly manifested as singularities in spatial coordinates and freezing of time coordinates. This paper points out that if the symmetry condition is replaced from "spherical symmetry in space" to "uniform symmetry in time", another class of exact solutions to the Einstein field equations can be obtained. In this solution, singularities appear in the time coordinate while spatial coordinates tend to diverge. This paper defines such solutions as "time black holes" and presents their metric form, horizon conditions, and physical implications. This model provides a geometric framework for understanding the origin of time, the end of time, and extreme time distortion phenomena.
Q Chen (Fri,) studied this question.