BekensteinHawkingEntropie

Bekenstein-Hawking entropy is a concept in theoretical physics that describes the entropy of a black hole. It was independently proposed by Jacob Bekenstein and Stephen Hawking in the 1970s. Entropy is a measure of the disorder or randomness in a system, and in the context of black holes, it refers to the amount of information that is lost when matter or energy falls into the black hole and is no longer accessible to the outside universe.

The Bekenstein-Hawking entropy formula is given by S = (A/4) * (c^3 / (G * h * k)), where S is the entropy, A is the area of the event horizon (the boundary of the black hole from which nothing can escape), c is the speed of light, G is the gravitational constant, h is the Planck constant, and k is the Boltzmann constant. This formula suggests that the entropy of a black hole is proportional to the area of its event horizon, rather than its volume or mass.

The significance of Bekenstein-Hawking entropy lies in its implications for the information paradox, which arises from the apparent loss of information when matter or energy falls into a black hole. According to quantum mechanics, information cannot be destroyed, but the information that falls into a black hole seems to be lost forever. The Bekenstein-Hawking entropy formula suggests that the information is not lost, but rather encoded in the entropy of the black hole's event horizon.

However, the exact nature of this encoding and how it resolves the information paradox remains an active area of research in theoretical physics. Despite this uncertainty, the Bekenstein-Hawking entropy formula has become a cornerstone of modern black hole physics and has been confirmed by numerous observations and experiments.