 We have seen how massive objects bend light. Einstein's general relativity theory shows that the more massive an object is, and the smaller its radius, the greater the bending. If we were looking at light passing close to a white dwarf, we would see that the bending is 50 times greater than we get with our sun. With a large enough mass and a small enough radius, like a neutron star, we actually get more than 360 degrees. In other words, the light might orbit the object several times before escaping and moving on to its final destination. So it's not a stretch to see that if the mass is large enough and the radius is small enough, light passing by close enough could enter a long-lasting orbit or never get out. And with enough mass, light emitted by the object itself would also be stuck inside. Nothing including light itself can escape. Hence the name black hole. In this segment, we'll cover how black holes are categorized and how they form. We'll cover their structure and the various ways they grow. We'll cover the first image of a black hole ever recorded. We'll cover examples from nearby black holes in our own galaxy to the most distant black hole ever discovered. And we'll end with coverage of a new theory for how the first black holes may have formed. A theory driven by the fact that the James Webb Space Telescope has found large galaxies that existed before the current Lambda cold dark matter cosmology predicted they would.