description Bekenstein-Hawking entropy Overview
The Bekenstein-Hawking entropy describes a fundamental property of black holes. It posits that a black hole’s information content is directly related to the surface area of its event horizon. This concept links gravity and quantum mechanics, suggesting that black holes harbor an immense number of internal configurations—microstates—despite their seemingly simple external appearance. Physicists and cosmologists studying black hole thermodynamics and the intersection of general relativity with quantum theory find this relationship particularly significant.
help Bekenstein-Hawking entropy FAQ
What does Bekenstein-Hawking entropy say about a black hole?
It says a black hole has entropy proportional to the area of its event horizon, not to its volume. The standard formula is S = k A c^3 / 4 G hbar, linking thermodynamics, gravity, and quantum theory.
Why is the area law surprising?
Most ordinary systems store entropy roughly with volume because their internal states fill space. A black hole instead scales with horizon area, which helped inspire the holographic principle in theoretical physics.
What did Jacob Bekenstein and Stephen Hawking each contribute?
Jacob Bekenstein argued in the 1970s that black holes should have entropy. Stephen Hawking then showed that black holes radiate thermally, giving the area-entropy idea a physical temperature.
How is Bekenstein-Hawking entropy related to the information paradox?
If a black hole has entropy, it appears to have many hidden microstates even though classical general relativity describes it mainly by mass, charge, and spin. The information paradox asks what happens to those microstates when Hawking radiation makes a black hole evaporate.
explore Explore More
Similar to Bekenstein-Hawking entropy
compare_arrows Compare: Hawking radiation See all arrow_forward
Reviews & Comments
Write a Review
Be the first to review
Share your thoughts with the community and help others make better decisions.
