Electromagnetic energy emitted by an object due to its temperature.

An idealized object that absorbs all incoming radiation and emits energy based solely on its temperature.

The wavelength at which a blackbody emits the most radiation is inversely proportional to its temperature.

The total power emitted by a blackbody is proportional to its surface area and the fourth power of its absolute temperature.

The constant that relates the energy of a photon to its frequency ($h \approx 6.626 \times 10^{-34} , \text{J} \cdot \text{s}$).

The prediction of classical physics that a blackbody would emit infinite energy at short wavelengths.

Classical physics failed to explain the blackbody spectrum, leading to the ultraviolet catastrophe. Planck's quantum approach introduced quantized energy, resolving the issue.

As temperature increases, the peak wavelength shifts to shorter wavelengths (blue shift), and the total power emitted increases significantly.

Increasing the surface area of a blackbody directly increases the total power emitted, as described by the Stefan-Boltzmann Law (P = AσT⁴).