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Black Holes: Physics, Structure, and Theory

1Introduction to Black Holes and Historical Context2Foundations of General Relativity3The Schwarzschild Solution4Geometry of Spacetime and Tidal Forces5Rotating Black Holes: The Kerr Metric6Black Hole Thermodynamics7Hawking Radiation and Quantum Effects8The Information Paradox9Formation and Astrophysical Evidence10Direct Imaging and Future Horizons
Introduction to Black Holes and Historical Context

What is a Black Hole?

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Let us begin by defining our subject. A black hole is not merely a dark object; it is a region of spacetime where gravity is so intense that nothing, not even light, can escape. This boundary is known as the event horizon. Once crossed, there is no return.
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Core Definition

A black hole is a region of spacetime exhibiting gravitational acceleration so strong that nothing—no particles or even electromagnetic radiation such as light—can escape from it. The boundary of no return is called the event horizon.

Why 'Black'?

Light cannot escape because the escape velocity required to overcome the gravitational pull exceeds the speed of light ($c$). Since nothing travels faster than $c$, nothing can leave.

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