The Stefan-Boltzmann Law is a physical law that describes the relationship between the temperature of an object and the amount of thermal radiation it emits. It states that the total energy radiated per unit surface area of an object is proportional to the fourth power of its absolute temperature.
The Stefan-Boltzmann Law was discovered by Austrian physicist Josef Stefan in 1879, and later refined by physicist Ludwig Boltzmann in 1884.
The formula for the Stefan-Boltzmann Law is I = σT^4, where I is the intensity of thermal radiation, σ is the Stefan-Boltzmann constant (5.67 x 10^-8 W/m^2K^4), and T is the absolute temperature of the object in Kelvin.
The Stefan-Boltzmann Law is used in various fields of science, such as astrophysics and thermodynamics, to calculate the thermal radiation emitted by objects at different temperatures. It is also used to study the behavior of stars and planets, as well as to design and improve technologies such as solar panels and infrared cameras.
The Stefan-Boltzmann Law has many practical applications, including measuring the surface temperature of stars, predicting the temperature of planets based on their distance from the sun, and calculating the amount of heat loss from buildings and other structures. It is also used in the development of thermal imaging devices and to study the thermal properties of materials.