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  1. Hawking radiation - Wikipedia

    Hawking radiation is dependent on the Unruh effect and the equivalence principle applied to black-hole horizons. Close to the event horizon of a black hole, a local observer must …

  2. This is the mathematical basis for Hawking radiation. We will need to (a) study asymptotic of u(t = 0) when ! +1 and (b) compute a certain functional E(u(t = 0)) where E is the vacuum quantum …

  3. Hawking Radiation - JILA

    Feb 3, 2018 · Classically, black holes are black. Quantum mechanically, black holes radiate, with a radiation known as Hawking radiation, after the British physicist Stephen Hawking who first …

  4. Hawking radiation | Black Holes, Quantum Mechanics, Particle …

    Nov 5, 2025 · Stephen W. Hawking proposed in 1974 that subatomic particle pairs (photon s, neutrino s, and some massive particles) arising naturally near the event horizon may result in …

  5. We derive the Hawking radiation power equations for black holes in asymptotically flat, asymptotically Anti-de Sitter (AdS) and asymptotically de Sitter (dS) black holes.

  6. Hawking Radiation - uni-hamburg.de

    In this note, we will review the derivation of Hawking e ect for an eternal Schwarzschild black hole in the framework of algebraic quantum eld theory.

  7. Hawking radiation explained in simple terms - BBC Sky at Night …

    Jan 24, 2024 · One of Professor Stephen Hawking’s most famous ideas is known as Hawking radiation. By leaking particles back into space, a black hole can very slowly evaporate away. …

  8. In this paper, we revisit the back-reaction problem and present a new approach for its solution.

  9. Hawking Radiation | Definition, Equation & Discovery - Study.com

    May 17, 2025 · Discover Hawking Radiation: its definition, equation, and how Stephen Hawking's theory explains black hole evaporation and challenges within classical physics. Updated: …

  10. Let's now derive some properties of Hawking radiation using math Recall that the Schwarzschild metric (32.1) has a coordinate singularity at the horizon r = rs Let's focus on the region close to …