Schwarzschild null geodesics
Schwarzschild Black Hole
Trace light at the edge of a horizon, where familiar intuition falls away.
Launch Simulation ↗
CAPTURED IN TUDUNI LABORATORYTHE PHYSICS
A closer look.
The horizon radius of a nonrotating, isolated black hole grows linearly with mass.
rₛ = 2GM / c²
G is the gravitational constant, M and m are masses, r is separation, c is the speed of light, and b is impact parameter where applicable.
What you can learn
- Explore the photon sphere and shadow
- Trace captured and escaping photons
- Separate physical lensing from display metaphors
Default bodies
One 10-solar-mass Schwarzschild black hole and a light emitter
CAPTURED IN TUDUNI LABORATORYNull geodesics assume a stationary, isolated, spherical, nonrotating black hole. Disk emissivity and fabric are illustrative; the N-body universe remains Newtonian.
Space fabric illustrates gravitational influence; it is not a numerical solution of the full Einstein field equations. Visual sizes can be enlarged independently of physical collision radii.