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 constant (b ≈ 2.898 x 10⁻³ m⋅K) that relates the peak wavelength of emitted radiation to the temperature of a blackbody.

The constant (σ ≈ 5.67 x 10⁻⁸ W m⁻² K⁻⁴) that relates the total power emitted by a blackbody to its surface area and temperature.

The constant (h) that relates the energy of a photon to its frequency (E = hf).

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

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.

A blackbody reaches thermal equilibrium when it emits the same amount of energy it absorbs, maintaining a constant temperature.

Energy is emitted in discrete packets (quanta) called photons, with energy E = hf, where h is Planck's constant and f is the frequency.