Stefan-Boltzmann Law The Stefan-Boltzmann law provides an empirical relationship between the temperature of a body and the rate at which it emits radiation....
The Stefan-Boltzmann law provides an empirical relationship between the temperature of a body and the rate at which it emits radiation. It states that the total radiated energy per unit surface area of a body is proportional to the fourth power of the body's temperature. In other words, the hotter a body is, the more radiation it emits.
Example: The Stefan-Boltzmann law is used to calculate the amount of radiation emitted by a star. The star's temperature is known, and its surface temperature can be inferred from this information.
Wien's displacement law describes the relationship between the wavelength of maximum emission of a body and its temperature. It states that the wavelength of maximum emission is inversely proportional to the temperature of the body. This means that the shorter the wavelength of maximum emission, the higher the temperature of the body.
Example: Wien's displacement law is used to study the color of stars. By measuring the wavelength of maximum emission, astronomers can infer the surface temperature of stars.
The Newton's law of cooling describes how the rate of cooling of an object is proportional to the difference between the object's temperature and the ambient temperature. This law states that the rate of cooling is directly proportional to the temperature difference between the object and the surroundings.
Example: The Newton's law of cooling is used to explain how objects cool down when they are placed in a colder environment. The law allows scientists to predict the rate at which an object will cool down