When two nuclei merge, such as in the case of a neutron star merger, their physical properties differ significantly based on their mass, density, and composition. Each nucleus possesses a unique gravitational pull and internal structure, which dictates how they interact as they approach one another during the collision process.
The outcome of such a merger depends heavily on the initial momentum and the total mass involved. In many astrophysical scenarios, the two bodies do not simply merge instantly. Instead, they undergo a complex process of tidal disruption and intense gravitational interaction. If the combined mass does not exceed a specific limit, the remnants may eventually coalesce into a single, stable core, such as a larger neutron star.
However, if the combined mass is too great, the gravitational collapse may be too rapid to maintain stability. In these instances, the merging nuclei may collapse further to form a black hole instead of a stable core. The specific physical characteristics of the original nuclei determine whether the result is a single stable object or a gravitational collapse into a singularity.
