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)
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
8th Edition
ISBN:9781259696527
Author:J.M. Smith Termodinamica en ingenieria quimica, Hendrick C Van Ness, Michael Abbott, Mark Swihart
Publisher:J.M. Smith Termodinamica en ingenieria quimica, Hendrick C Van Ness, Michael Abbott, Mark Swihart
Chapter1: Introduction
Section: Chapter Questions
Problem 1.1P
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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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