The Stefan–Boltzmann law, also known as Stefan's law, states that the total energy radiated per unit surface area of a black body in unit time (known variously as the black-body irradiance, energy flux density, radiant flux, or the emissive power), j*, is directly proportional to the fourth power of the black body's
The Stefan-Boltzmann law states that the total thermal energy radiated per unit surface area of a black body in thermal equilibrium (i.e., at a constant temperature) is proportional to the fourth power of its absolute temperature. Mathematically, it can be expressed as:
E = σ * T^4
where E is the energy radiated per unit surface area, σ is the Stefan-Boltzmann constant, and T is the temperature of the black body in Kelvin. The law is a fundamental principle in thermal physics and has many practical applications in fields such as astronomy, engineering, and climate science.
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Answer:
The Stefan–Boltzmann law, also known as Stefan's law, states that the total energy radiated per unit surface area of a black body in unit time (known variously as the black-body irradiance, energy flux density, radiant flux, or the emissive power), j*, is directly proportional to the fourth power of the black body's
Explanation:
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Answer:
The Stefan-Boltzmann law states that the total thermal energy radiated per unit surface area of a black body in thermal equilibrium (i.e., at a constant temperature) is proportional to the fourth power of its absolute temperature. Mathematically, it can be expressed as:
E = σ * T^4
where E is the energy radiated per unit surface area, σ is the Stefan-Boltzmann constant, and T is the temperature of the black body in Kelvin. The law is a fundamental principle in thermal physics and has many practical applications in fields such as astronomy, engineering, and climate science.
Explanation: