Black Hole Collision Calculator

This calculator relies on fundamental laws of gravitation, mass-energy equivalence, and general relativity. First, the Schwarzschild radius ($r_s$) of any mass ($M$) is determined by the formula $r_s = \frac{2GM}{c^2}$, where $G$ is the gravitational constant and $c$ is the speed of light. When an object or secondary black hole of a specific mass is consumed, roughly 7% of its rest-mass energy is converted into gravitational waves, yielding the energy release formula $E = \Delta m \cdot 0.07 \cdot c^2$. Furthermore, the final mass accounts for an efficiency retention factor, while gravitational fields and potential energy shifts are mapped across critical thresholds like the innermost stable circular orbit.

Imagine a primary supermassive black hole with an initial mass of $1,000,000$ solar units absorbing an incoming object with a mass eaten value of $50,000$ solar units. First, we compute the energy released during the inspiral and merger phase using $E = \Delta m \cdot 0.07 \cdot c^2$, which outputs a tremendous burst of gravitational wave energy. The final mass of the primary black hole increases by roughly $93\%$ of the consumed mass factor, leading to a new Schwarzschild radius calculated via $r_{s,\text{big}} = \frac{2GM_{\text{final}}}{c^2}$. The percentage difference between the initial and final event horizon radii can then be tracked precisely to understand spatial expansion.

When inputting large astronomical values, always verify your unit consistency—ideally converting solar masses or kilograms uniformly across all fields. Keep in mind that simplified Newtonian approximations for potential energy work well at safe distances, but extreme accuracy near the event horizon requires accounting for relativistic frame-dragging and nonlinear wave emission efficiencies.