Blackbody Radiation Simulation
Planck's law & Wien's displacement
Hotter objects emit more radiation and peak at shorter wavelengths. The Sun (~5778K) peaks in visible light. The colored circle shows the star's approximate color.
What Is Blackbody Radiation?
Blackbody Radiation refers to planck's law & wien's displacement in optics & light. This page visualizes the phenomenon with interactive controls so you can change parameters and observe how the model responds.
What To Observe
- Watch how the visual pattern or system response changes as you adjust the controls for Blackbody Radiation.
- Relate each visual change to the core phenomenon shown here: planck's law & wien's displacement.
- Use repeated runs with one parameter changed at a time to build intuition.
Related Simulations
Snell's Law (Refraction) Light bending at material boundaries Total Internal Reflection Critical angle and trapped rays at refractive boundaries Thin Lens Simulation Ray tracing and image formation with thin lenses Mirror Reflection (Concave/Convex) Curved-mirror ray diagrams and image properties Prism Light Dispersion White light split by wavelength-dependent refraction Rayleigh Scattering Shorter wavelengths scatter more strongly in the atmosphere Brewster's Angle P-polarized reflection vanishes at a special incidence angle Fresnel Diffraction Near-field diffraction pattern from phase summation Chromatic Aberration Different wavelengths focus at different image distances Thin Film Interference Reflected color varies with film thickness and angle Optical Fiber Light Guide Guiding by total internal reflection in a core-cladding fiber
Try These Experiments
- Start with default settings, then change one slider at a time.
- Record what increases, decreases, or becomes unstable as parameters vary.
- Use screenshots or notes to compare patterns between runs.
Real-World Applications
- Optics & Light lessons and classroom demonstrations
- Self-study and concept reinforcement
- Interactive support for STEM presentations