Related Experiment Video
Updated: Jun 7, 2025
05:39
Scalable Quantum Integrated Circuits on Superconducting Two-Dimensional Electron Gas Platform
Published on: August 2, 2019
9.5K
Quantum Inequalities for Quantum Black Holes
Antonia M Frassino1,2,3, Robie A Hennigar2, Juan F Pedraza4
1Departamento de Física y Matemáticas, <a href="https://ror.org/04pmn0e78">Universidad de Alcalá</a>, Campus Universitario, Alcalá de Henares, 28805 Madrid, Spain.
Physical Review Letters
|November 15, 2024
Summary
We developed new spacetime inequalities for quantum black holes that work in all dimensions and orders of backreaction. These findings support the existence of cosmic censorship and suggest a maximum entropy state for quantum black holes.
Area of Science:
- Theoretical physics
- Quantum gravity
- Black hole thermodynamics
Background:
- Semiclassical gravity describes quantum effects in black holes.
- Existing quantum Penrose inequalities are limited, failing in 3D beyond perturbative calculations.
- Understanding black hole behavior requires accounting for all orders of backreaction.
Purpose of the Study:
- To formulate new spacetime inequalities for quantum-corrected black holes.
- To propose refined quantum Penrose and reverse isoperimetric inequalities for 3D anti-de Sitter black holes.
- To investigate implications for cosmic censorship and black hole entropy.
Main Methods:
- Formulating spacetime inequalities in semiclassical gravity.
- Applying these inequalities to all orders of backreaction.
- Analyzing three-dimensional asymptotically anti-de Sitter quantum black holes.
Main Results:
- Developed quantum Penrose and reverse isoperimetric inequalities valid in 3D for all orders of backreaction.
- Demonstrated that the quantum Penrose inequality holds beyond the perturbative regime in 3D.
- Showed that the quantum reverse isoperimetric inequality implies a maximum entropy state for quantum black holes.
Conclusions:
- The proposed quantum Penrose inequality supports the existence of cosmic censorship in nonperturbative semiclassical gravity.
- The quantum reverse isoperimetric inequality suggests a limit on quantum black hole entropy for a fixed volume.
- These inequalities provide a new framework for studying quantum black holes.
Related Concept Videos
01:10Detection of Black Holes
2.2K
Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
Not until the 1960s, when the first neutron...
2.2K
01:21Schwarzschild Radius and Event Horizon
1.9K
No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
The minimum speed required to launch a projectile from the surface of an object to which it is gravitationally bound so that it eventually escapes the object’s gravitational field is called the escape velocity. The escape velocity is independent of the mass of the object. Merging the idea of escape...
1.9K
03:06The Pauli Exclusion Principle
35.2K
The arrangement of electrons in the orbitals of an atom is called its electron configuration. We describe an electron configuration with a symbol that contains three pieces of information:
35.2K
04:08The Uncertainty Principle
23.1K
Werner Heisenberg considered the limits of how accurately one can measure properties of an electron or other microscopic particles. He determined that there is a fundamental limit to how accurately one can measure both a particle’s position and its momentum simultaneously. The more accurate the measurement of the momentum of a particle is known, the less accurate the position at that time is known and vice versa. This is what is now called the Heisenberg uncertainty principle. He...
23.1K
02:43Quantum Numbers
34.3K
It is said that the energy of an electron in an atom is quantized; that is, it can be equal only to certain specific values and can jump from one energy level to another but not transition smoothly or stay between these levels.
34.3K
02:45The Quantum-Mechanical Model of an Atom
42.0K
Shortly after de Broglie published his ideas that the electron in a hydrogen atom could be better thought of as being a circular standing wave instead of a particle moving in quantized circular orbits, Erwin Schrödinger extended de Broglie’s work by deriving what is now known as the Schrödinger equation. When Schrödinger applied his equation to hydrogen-like atoms, he was able to reproduce Bohr’s expression for the energy and, thus, the Rydberg formula governing hydrogen spectra.
42.0K