Black Hole's Schwarzschild Radius - Definition and In-depth Explanation - Cosmic Phenomena Guidebook
The Schwarzschild Radius, a term coined by the German physicist Karl Schwarzschild in 1916, is a crucial aspect of black hole physics. This radius, calculated using the formula R_s = 2GM/c^2, where G is the gravitational constant, M is the mass of the black hole, and c is the speed of light in a vacuum, defines the boundary known as the event horizon.
Beyond this horizon, nothing, not even light, can escape the gravitational pull of the black hole. The Schwarzschild Radius marks the point of no return for any object that crosses it. It is a key concept in understanding the properties of black holes, such as their size, mass, and gravitational influence on their surroundings.
The Schwarzschild Radius is applicable to non-rotating, uncharged black holes. It plays a crucial role in determining the properties of these black holes, making it a fundamental aspect of the theory of general relativity.
However, the Schwarzschild Radius is not applicable to most objects in the universe due to their dispersed mass. Only when an object's mass is compressed to a certain critical density can it collapse into a black hole with a Schwarzschild Radius.
The larger the mass of the black hole, the larger its Schwarzschild Radius will be. For instance, all black holes with a Schwarzschild radius larger than Earth’s radius (approximately 6,371 km) have a mass exceeding about 2.74 times the mass of the Sun.
Once an object passes the Schwarzschild Radius and enters the event horizon of a black hole, it is inevitably pulled towards the singularity at the center of the black hole. At the Schwarzschild Radius, the gravitational pull becomes infinitely strong.
The Schwarzschild Radius is a direct proportion of the mass of the black hole. It is a key aspect of the theory of general relativity and a fundamental concept in the study of black holes.
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