Using the thermal radiation equation below and your knowledge of solar flux calculate the flux emitted from a star with a temperature of 6200 K to 2.d.p. Assume the star is a perfect black-body. The Stefan–Boltzmann thermal radiation equation is: P = AεσT4 Where P    = Power (W) A   = Surface area (m2) ε    = Emissivity σ    = The Stefan-Boltzmann constant is 5.67 x 10-8 W · m-2 · K-4 T    = Temperature (K)

Introduction to Chemical Engineering Thermodynamics
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Author:J.M. Smith Termodinamica en ingenieria quimica, Hendrick C Van Ness, Michael Abbott, Mark Swihart
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  a)     Using the thermal radiation equation below and your knowledge of solar flux calculate the flux emitted from a star with a temperature of 6200 K to 2.d.p. Assume the star is a perfect black-body. The Stefan–Boltzmann thermal radiation equation is: P = AεσT4 Where P    = Power (W) A   = Surface area (m2) ε    = Emissivity σ    = The Stefan-Boltzmann constant is 5.67 x 10-8 W · m-2 · K-4 T    = Temperature (K)
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