Stefan-Boltzmann law

This may be related to other properties of the object through the Stefan-Boltzmann law.

The denominator can also be recognized from the Stefan-Boltzmann law.

Stefan-Boltzmann law - The total flux emitted by a black body.

From the Stefan-Boltzmann law, this surface will radiate 460 watts.

Metamaterials may be designed to exceed the Stefan-Boltzmann law.

With the Stefan-Boltzmann law, astronomers can easily infer the radii of stars.

The Stefan-Boltzmann law gives an expression for the power radiated by the planet:

According to the Stefan-Boltzmann law, if temperature doubles, radiated energy increases by a factor of 16 (2 to the 4th power).

The surface of a star is defined to have a temperature given by the effective temperature in the Stefan-Boltzmann law.

The Stefan-Boltzmann law gives the total power (energy/second) the Sun is emitting:

The amount of heat a surface radiates is proportional to the fourth power of its temperature (the Stefan-Boltzmann law).

As radiators work at a relatively low temperature, the Stefan-Boltzmann law means that they are weak radiators of heat.

One thing I did not notice, though, is the Stefan-Boltzmann law (radiative energy transfer being proportional to the fourth power of temperature).

Light in thermal equilibrium has a black body spectrum with an energy density proportional to the fourth power of the temperature (hence the Stefan-Boltzmann law).

This appears when integrating Planck's law to derive the Stefan-Boltzmann law in physics.

Since the planet is also a black body which emits radiation according to the Stefan-Boltzmann law, it will emit radiation and lose energy.

For a black body, for example, the spectrally integrated intensity is proportional to the fourth power of the temperature (Stefan-Boltzmann law).

The Stefan-Boltzmann law is discovered by Jozef Stefan.

The Stefan-Boltzmann law, also known as Stefan's law, is a relation which described the power radiated from a black body in terms of its temperature.

Pyranometer principle: solar radiation flux density relates to surface temperature (Stefan-Boltzmann law)

(the Stefan-Boltzmann law and Wien approximation in physics)

The surface emits a radiative flux density F according to the Stefan-Boltzmann law:

The total radiative intensity of a black body rises as the fourth power of the absolute temperature, as expressed by the Stefan-Boltzmann law.

Wien's law gives the most likely frequency of the emitted radiation, and the Stefan-Boltzmann law gives the heat intensity.

As established by the Stefan-Boltzmann law, the intensity of black-body radiation increases as the fourth power of absolute temperature.