The Dynamic Evolution of Black Holes in General Relativity: Numerical Relativity Simulation

Abstract

As the core of the star left behind by the supernova explosion continues to collapse, the immense pressure causes protons to absorb electrons and transform into electrically neutral neutrons. The core of the star eventually forms a dense neutron star about 10 kilometres across, much smaller than a city. Neutron stars resemble giant atomic nuclei and are much denser than any atomic material on Earth. A small cup of matter from a neutron star exceeds the total mass of everyone on Earth. If the mass of the star's core is large enough, it will continue to collapse beyond the Schwarzschild radius, eventually forming a black hole. The gravitational field of a black hole is so strong that neither matter nor electromagnetic waves (including visible light) can escape from it. The boundary of this inescapable region is called the event horizon. In our experiments, we used a high-performance computing cluster and numerical relativity simulation software to accurately solve Einstein's field equations and demonstrate that the peak amplitude of gravitational waves emitted by black holes during mergers can reach with a frequency of 300 Hz. This study provides important insights into the dynamic evolution of black holes and the emission of gravitational waves under various initial conditions.