Model blackbody emission with Planck’s radiation law precisely. Choose wavelength limits, step size, and units. See peak shifts as temperature rises across spectra clearly.
| Temperature (K) | Wavelength (nm) | Spectral radiance (W·sr⁻¹·m⁻²·nm⁻¹) | Notes |
|---|---|---|---|
| 300 | 10000 | ≈ 9.9e-3 | Thermal infrared dominates at room temperature. |
| 1000 | 3000 | ≈ 1.1e+2 | Peak moves toward near-infrared with heating. |
| 5800 | 500 | ≈ 2.6e+7 | Visible band becomes strong for solar-like temperatures. |
Planck’s law describes the spectral radiance of an ideal blackbody at temperature T. This calculator supports both wavelength and frequency forms.
Constants used: Planck constant h, speed of light c, and Boltzmann constant k in SI units.
Important Note: All the Calculators listed in this site are for educational purpose only and we do not guarentee the accuracy of results. Please do consult with other sources as well.