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ਸੋਨੀ ਸਿੰਘ ਭੜ੍ਹੌ - Author on ShareChat: Funny, Romantic, Videos, Shayari, Quotes
ਸੋਨੀ ਸਿੰਘ ਭੜ੍ਹੌ
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#📜 ਜਨਰਲ ਨੌਲਜ #🔍 ਰੌਚਕ ਤੱਥ 🔖 #💡 ਜਾਣਕਾਰੀ ਸਪੈਸ਼ਲ #📖 ਐਜੂਕੇਸ਼ਨਲ ਫੋਟੋਆਂ/ਵੀਡਿਓਜ਼ 📔 #🧐ਫ਼ੈਕਟਸ
📜 ਜਨਰਲ ਨੌਲਜ - Stefan - Boltzmann Law Total Power of Blackbody Radiation The Stefan - Boltzmann law states that the total radiant power emitted per unit area of a blackbody is proportional to the fourth power of its absolute temperature . = στ4 ( radiant exitance of a blackbody ) P = σ AT 4 ( total radiant power ) Key Points A heated blackbody surface Radiant emits radiation Exitance in all directions . ( W / m² ) • The total radiant exitance of a blackbody is proportional to T. As temperature increases , the emitted power increases very rapidly . This law applies ideally to blackbodies . • Real surfaces emit less : j = εσT + ( 0≤E≤1 , emissivity ) Why it Matters ? The Stefan - Boltzmann law connects temperature with thermal radiation , helping us understand how hot objects lose energy by emitting radiation . j * P Meaning of Symbols = radiant exitance = σ = > A = = total power Stefan - Boltzmann constant 5.670 x 108 W m - 2 K - 4 area T = absolute temperature ( K ) Radiant exitance increases rapidly with temperature ( proportional to T * ) . → T ( K ) Josef Stefan 1835-1893 Austrian Physicist Ludwig Boltzmann later provided the theoretical derivation of this law . Real - World Applications Energy output of stars Design and analysis of furnaces Thermal cameras and infrared imaging • Climate studies and Earth's radiation balance - ShareChat