Blackbody fraction of Radiation

AI Thread Summary
The discussion revolves around calculating the fraction of energy radiated by the sun in the visible spectrum (350 nm to 700 nm) using the Stefan-Boltzmann law and Planck's law of black body radiation. Participants emphasize that the Stefan-Boltzmann law alone is insufficient for this specific calculation, as it provides total intensity rather than spectral distribution. Instead, integration of the Planck function over the specified wavelength range is necessary. One user expresses frustration with obtaining a zero result from their calculations, indicating a potential error in their integration process. The conversation highlights the importance of correctly applying the relevant equations and methods to solve the problem accurately.
patapat
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Homework Statement


Determine the fraction of the energy radiated by the sun in the visible region of the spectrum (350 nm to 700 nm). (Assume the sun's surface temperature is 5800 K.)


Homework Equations


R=\sigmaT^{4}

for some reason i can't make the sigma come down, but it's a constant=5.67x10^{-8}W/m^{2}K^{4}

The Attempt at a Solution


I'm not sure if the blackbody radiation equation is relevant, but I'm not sure where to begin with this.
 
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patapat said:

Homework Statement


Determine the fraction of the energy radiated by the sun in the visible region of the spectrum (350 nm to 700 nm). (Assume the sun's surface temperature is 5800 K.)


Homework Equations


R=\sigmaT^{4}

for some reason i can't make the sigma come down, but it's a constant=5.67x10^{-8}W/m^{2}K^{4}

The Attempt at a Solution


I'm not sure if the blackbody radiation equation is relevant, but I'm not sure where to begin with this.


This formula (the Stefan-Boltzmann law) you gave gives the intensity radiated at all wavelength. so it's useless for your question. You need the function I(\lambda,T) which you will have to integrate over the range of wavelength provided (and you could check that integrating from 0 to infinity would reproduce the SB law).

Hope this helps
 
http://en.wikipedia.org/wiki/Planck's_law_of_black_body_radiation

Then you perform the integration between 350 and 700, then compare the result with the integration from 0 to infinity.

Hint: That last result is also know as a "theorem", what is it called and how does it look like?
 
I'm working this same problem right now, and have done everything suggested (and then some), but even using maple to integrate I keep getting that the definite integral comes out to approx. 0 - 0 = 0. This is obviously wrong since more than zero energy gets radiated in the visible portion.

Converting the energy density function to 8pi*hc(kT/hc)^4*int(x^3/(e^x-1)) using
x = hc/lambda*kT, Maple gives me the antiderivative [of int(x^3/(e^x-1))] to be -1/4x^4 + x^3*ln(e^x-1) + 3x^2*polylog(2,e^x) - 6x*polylog(3,e^x) + 6*polylog(4,e^x). Converting 350 nm and 700 nm to values of x and evaluating gives the 0 answer.

Can anyone point out what retarded mistake I must be making? Also sorry about typing the formulas out like that but I haven't figured out how to format it yet.
 
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