What is the energy density of sunlight on Earth and near the surface of the sun?

AI Thread Summary
The discussion focuses on calculating the energy density of sunlight at Earth and near the surface of the sun using the solar constant of 1350 W/m^2. The Stefan-Boltzmann law and solar luminosity equations are referenced for these calculations. Participants express frustration with the application of these formulas and seek clarification on using Planck's formula or Rayleigh-Jeans law for their calculations. The energy density on Earth is derived from the solar constant, while the energy density near the sun's surface involves calculating luminosity and applying the appropriate formulas. Overall, the thread highlights the challenges faced in applying theoretical physics to practical problems.
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[SOLVED] Energy Density of Sunlight

Homework Statement


Use the solar constant (1350 W/m^2) to calculate the energy density of sunlight at a)Earth and b) near the surface of the sun.


Homework Equations


Stefan-Boltzman = (2pi^5)/(15(h^3)(c^2))
h=6.63x10^-34 j.s
L(solar luminosity)=4pi(D^2)S
S=1340 W/m^2


The Attempt at a Solution


I don't know what I'm doing. I'm assuming those are the more important things to use.
I'm getting frustrated with this and really need some help. I'm trying to plug in the power per area into the stefan boltzman eq to see if I can find the answer but it isn't working.
 
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Thought about it some...

Could I use Planks formula or Raleight Jeanes law to solve this? Since the wavelength is rather large, I'm thinking I could, but I'm not sure how to apply it.
 
Last edited:
dR/D(lambda)=dU/d(lambda)(4/c)
du=4dR/c
integrate
u=4R/c

where R is 1350(solar constant) and gives the energy density on earth.

for part b

L=4pir^2 S(solar constant)
S=L(luminosity)/4pir(of the sun)^2
then u=4r/c where R=S
 
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