This simulator visualizes how a uniformly accelerating observer's Rindler horizon splits spacetime into causally disconnected wedges, and how the entangled vacuum state, perfectly empty to an inertial observer, decomposes into a thermal bath of particles whose temperature scales directly with the chosen proper acceleration.
Adjust the proper acceleration slider to see the observer's hyperbolic Rindler trajectory and horizon shift on the spacetime diagram, and watch the corresponding Unruh temperature and blackbody-like particle spectrum update in real time. Toggle between the inertial observer's view of the vacuum and the accelerated observer's view to compare how the same physical state is described differently, and switch on the horizon-entanglement overlay to see the two-mode pairing between accessible and inaccessible field modes.
Slider for proper acceleration magnitude; toggle to switch between inertial-frame and Rindler-frame (accelerated observer) views; toggle to show or hide the horizon-entanglement mode-pairing overlay; readout panel displaying computed Unruh temperature and a sample thermal particle spectrum.
To reach a detectable Unruh temperature of just one kelvin, an observer would need a sustained acceleration of roughly ten to the twenty power meters per second squared, tens of trillions of times greater than the acceleration felt in the most extreme centrifuges or particle-collider bending magnets on Earth.
This simulator visualizes how a uniformly accelerating observer's Rindler horizon splits spacetime into causally disconnected wedges, and how the entangled vacuum state, perfectly empty to an inertial observer, decomposes into a thermal bath of particles whose temperature scales directly with the chosen proper acceleration.
This simulator visualizes how a uniformly accelerating observer's Rindler horizon splits spacetime into causally disconnected wedges, and how the entangled vacuum state, perfectly empty to an inertial observer, decomposes into a thermal bath of particles whose temperature scales directly with the chosen proper acceleration.
Adjust the proper acceleration slider to see the observer's hyperbolic Rindler trajectory and horizon shift on the spacetime diagram, and watch the corresponding Unruh temperature and blackbody-like particle spectrum update in real time. Toggle between the inertial observer's view of the vacuum and the accelerated observer's view to compare how the same physical state is described differently, and switch on the horizon-entanglement overlay to see the two-mode pairing between accessible and inaccessible field modes.
To reach a detectable Unruh temperature of just one kelvin, an observer would need a sustained acceleration of roughly ten to the twenty power meters per second squared, tens of trillions of times greater than the acceleration felt in the most extreme centrifuges or particle-collider bending magnets on Earth.