8 Space & Relativity Visualizations That Will Transform How You See the Universe

Black holes evaporate. Time slows down near light speed. Starlight bends as it grazes massive objects. These aren't science fiction—they're verified predictions of modern physics, running live in your browser.

ElysiaTools just released a collection of interactive space and relativity visualizations. No downloads. No sign-up. Just open and explore.

1. Black Hole Hawking Radiation

Nothing in the universe lasts forever—not even black holes.

Stephen Hawking showed that black holes aren't completely black. At the event horizon, quantum effects create virtual particle pairs: one falls into the black hole, the other escapes as Hawking radiation. The escaping particle carries away energy, so the black hole slowly loses mass over time.

Smaller black holes evaporate faster. A black hole the mass of our Sun would take 10⁶⁷ years to evaporate completely—far longer than the age of the universe. But primordial black holes, if they exist, might be evaporating right now, spitting out particles in their final seconds.

This visualization lets you drop a black hole's mass, watch the evaporation curve in real time, and see the power output change as the black hole shrinks. You can toggle the accretion disk, relativistic jets, and the photon sphere. Presets cover stellar black holes, primordial black holes, and the final explosion phase.

👉 Try Black Hole Hawking Radiation

2. Planetary Orbit Simulation

Planets don't travel in circles. They trace ellipses, with the Sun sitting at one focus.

This interactive simulation applies Newton's law of gravitation and Kepler's three laws of planetary motion in real time. Watch energy exchange as a planet speeds up near perihelion and slows down at aphelion. Enable multi-body mode and see three planets perturb each other's orbits, occasionally destabilizing into chaos.

The simulation tracks total mechanical energy, angular momentum, and orbital velocity at every point. Toggle velocity vectors, orbital trails, and zoom in or out to see the full picture—or zoom down to watch intimate gravitational interactions.

👉 Try Planetary Orbit Simulation

3. Time Dilation Visualization

Move fast enough, and time moves slower for you relative to everyone else. That's time dilation—not a metaphor, not a trick. It's how reality works.

Einstein's special relativity predicts that a moving clock ticks slower by a factor of γ = 1/√(1 − v²/c²). At 50% of light speed, γ = 1.15. At 90%, γ jumps to 2.29. At 99%, it's 7.09. Approach light speed and γ approaches infinity—in theory, time stops.

This visualization shows two synchronized clocks: one stationary, one moving. Watch them drift apart as you push the velocity slider up. The Lorentz factor curve plots γ vs. v/c in real time. It also explains the famous twin paradox—why the traveling twin ages less than the twin who stayed home.

Real-world proof: GPS satellites tick 38 microseconds faster per day due to their orbital speed (time dilation) but 45 microseconds slower due to weaker gravity (gravitational blueshift). The net effect is −7 μs/day, which must be corrected or GPS drifts by 10 km daily.

👉 Try Time Dilation Visualization

4. Stellar Aberration Visualization

When you walk through rain, you tilt your umbrella forward. Light works the same way—but at 107,000 km/h (Earth's orbital speed), the effect on starlight is measurable.

Stellar aberration causes stars to appear displaced in the direction of Earth's motion around the Sun. British astronomer James Bradley discovered it in 1725 while trying to measure stellar parallax. He didn't find parallax (stars are too far), but he found something stranger: stars trace small ellipses over the course of a year, shifted 20 arcseconds from their true position.

This visualization shows the sky as seen from a stationary frame versus a moving one. Drag the velocity slider from 0 to 0.99c and watch the star field compress toward the direction of motion—the relativistic headlight effect. At 99% of light speed, 180° of sky collapses into about 8°.

This effect is critical for satellite navigation and high-precision astrometry. GPS must account for it.

👉 Try Stellar Aberration Visualization

5. Tyndall Effect

Why can you see a laser beam through milk but not through salt water?

The Tyndall effect is light scattering by particles in a colloid. Suspended particles (10–1000 nm) scatter short-wavelength light more than long-wavelength light, making the beam visible from the side. In a true solution (dissolved ions, <1 nm), no scattering occurs—the beam is invisible.

This interactive simulation lets you compare a colloid, true solution, and suspension side by side. Choose laser wavelength (red, green, blue, or white) and watch the scattering intensity change. The Rayleigh scattering formula shows why the sky is blue (short wavelengths scatter most) and why sunsets are red (long wavelengths survive scattering at low angles).

Try the colloidal gold preset and watch the red light scatter with an eerie orange glow—the same effect that makes stained glass windows shimmer.

👉 Try Tyndall Effect Visualization

6. Prism Dispersion

Isaac Newton performed this experiment in 1666. Take a beam of white light. Pass it through a glass prism. Watch it fan out into red, orange, yellow, green, blue, violet.

Dispersion happens because the refractive index of glass varies with wavelength. Short wavelengths (violet, ~400 nm) bend more than long wavelengths (red, ~700 nm). The difference is small in glass, but over the full visible spectrum, it produces the familiar rainbow.

This simulation lets you dial in the prism material (crown glass, flint glass, diamond), apex angle, and incident angle. Watch the spectrum emerge in real time with angle labels and deviation values for each wavelength. The Abbe number controls dispersion strength—diamond has a low Abbe number (~55), meaning it disperses strongly, which is why diamonds sparkle with fire.

Rainbows are formed by dispersion in millions of water droplets, each acting as a tiny prism. The secondary rainbow (with colors reversed) occurs from light reflecting twice inside each droplet.

👉 Try Prism Dispersion Simulation

7. Total Internal Reflection

You can trap light inside glass—but only if you hit the right angle.

Total internal reflection (TIR) occurs when light travels from a denser medium (n₁) to a rarer medium (n₂) at an angle exceeding the critical angle θ꜀ = arcsin(n₂/n₁). Every photon reflects back into the denser medium. No refraction. 100% efficiency.

For glass to air, θ꜀ ≈ 41.8°. For diamond to air, θ꜀ ≈ 24.4°. Diamond's high refractive index and low critical angle are why diamonds are cut to maximize TIR—the light bounces around inside, only exiting through the top facets.

This visualization shows the critical angle in action. Drag the incident angle slider and watch the switch from refraction to total reflection. Then switch to fiber optic mode and see how TIR enables fiber optic communication—light bounces down a glass fiber over thousands of kilometers with minimal loss. This is the backbone of the modern internet.

👉 Try Total Internal Reflection

8. Photoelectric Effect

This experiment broke classical physics—and birthed quantum mechanics.

Classically, light is a wave. Crank up the intensity and electrons should fly out with more energy. But Heinrich Hertz discovered something else in 1887: below a certain threshold frequency, no electrons escape—no matter how bright the light. Above the threshold, electrons pop out instantly, and their energy depends only on frequency, not intensity.

Einstein explained it in 1905 (his Nobel Prize paper): light comes in packets called photons. Each photon's energy is E = hf, where h is Planck's constant and f is frequency. One photon kicks out one electron—if and only if hf exceeds the metal's work function. Intensity just means more photons, not more energy per photon.

This simulation lets you tune the light frequency and intensity, choose the metal (sodium, cesium, aluminum, gold), and watch the I–V curve form in real time. The cutoff voltage, threshold frequency, and work function all become tangible. At the threshold, electrons barely escape. Increase frequency and watch them rocket off.

👉 Try Photoelectric Effect Visualization

The Unfinished Problem

These eight visualizations reveal a universe stranger than Newton imagined. But one question remains stubbornly open: what happens at the center of a black hole?

General relativity predicts a singularity—infinite density, zero volume, the end of spacetime. But infinities in physics usually mean the theory broke down, not that reality did. Quantum gravity (string theory, loop quantum gravity) is attempting to replace the singularity with something finite. Some models suggest a "bounce"—the black hole compresses matter to extreme density, then rebounds outward into a new universe.

We don't know yet. That's what makes physics worth doing.