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trou n Cas 1 I, di cos² 0 dN C J sphere Prad.A di = (transmis: || les 1 2л I, dr cos² 0 sin 0 d0 dø $=0 Je=0 -In dr por 3c (isotropic radiation fielo er, it may be that the radiation field is not isotropic. In that c |

trou n Cas 1 I, di cos² 0 dN C J sphere Prad.A di = (transmis: || les 1 2л I, dr cos² 0 sin 0 d0 dø $=0 Je=0 -In dr por 3c (isotropic radiation fielo er, it may be that the radiation field is not isotropic. In that c |

Principles of Heat Transfer (Activate Learning with these NEW titles from Engineering!)
Principles of Heat Transfer (Activate Learning with these NEW titles from Engineering!)
8th Edition
ISBN:9781305387102
Author:Kreith, Frank; Manglik, Raj M.
Publisher:Kreith, Frank; Manglik, Raj M.
Chapter1: Basic Modes Of Heat Transfer
Section: Chapter Questions
Problem 1.24P: Two large parallel plates with surface conditions approximating those of a blackbody are maintained...
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Attached is the question and the formula to solve it. I attached the formula directly from the book, the Blackbody radiation Pressure formula that is. Thank you :)

isotropic radiation field, there will be no change in the expression for the radiation p if the leading factor of 2 (which originated in the change in momentum upon refle the photons) is removed and the angular integration is extended over all solid angl = YP Y'pe sphere vloupin UP O „S0ɔ Yp YI (transmission) - C by CAGE I, dì cos² 0 sin 0 d0 dø by 1. C. –I, d. (isotropic radiation field). However, it may be that the radiation field is not isotropic. In that case, Eq. (9.9) diation pressure is still valid but the pressure depends on the orientation of the ma surface d A. The total radiation pressure produced by photons of all wavelengths is fou grating Eq. (9.10): = Pe Prad Prad,à dr. %D For blackbody radiation, it is left as a problem to show that (ma) dpofave 40 T4 B(T) da aT 1. -u. %3D %3D hus the blackbody radiation pressure is one-third of the energy density. (Fo e pressure of an ideal monatomic gas is two-thirds of its energy density.) 266 BAPUAll
Transcribed Image Text:isotropic radiation field, there will be no change in the expression for the radiation p if the leading factor of 2 (which originated in the change in momentum upon refle the photons) is removed and the angular integration is extended over all solid angl = YP Y'pe sphere vloupin UP O „S0ɔ Yp YI (transmission) - C by CAGE I, dì cos² 0 sin 0 d0 dø by 1. C. –I, d. (isotropic radiation field). However, it may be that the radiation field is not isotropic. In that case, Eq. (9.9) diation pressure is still valid but the pressure depends on the orientation of the ma surface d A. The total radiation pressure produced by photons of all wavelengths is fou grating Eq. (9.10): = Pe Prad Prad,à dr. %D For blackbody radiation, it is left as a problem to show that (ma) dpofave 40 T4 B(T) da aT 1. -u. %3D %3D hus the blackbody radiation pressure is one-third of the energy density. (Fo e pressure of an ideal monatomic gas is two-thirds of its energy density.) 266 BAPUAll
Derive the formula for the radiation pressure of a blackbody Prad starting from Prad = S° Ba(T)d2 . Use Planck's spectral radiance, the transformation of variable 3c hc and an integral table (easy to find online). akt x =
Transcribed Image Text:Derive the formula for the radiation pressure of a blackbody Prad starting from Prad = S° Ba(T)d2 . Use Planck's spectral radiance, the transformation of variable 3c hc and an integral table (easy to find online). akt x =
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