2. Can we Estimate the Solar Constant? A result from theoretical physics, known as theStefan-Boltzmann law, states that the total power radiated by a blackbody at temperature T (K)per unit surface area is given byE=GT*where E is radiated power per unit surface area of the blackbody and o is the Stefan-Boltzmannconstant equal to 5.67 x 10* Wm?K*. Let's assume that the sun is a perfect blackbody at T=5783 K and apply the laws of energy conservation to estimate the average incidence of solarenergy [W/m] arriving at the top of Earth's atmosphere (we call that incident energy the solarconstant). Compare your calculated estimate of the solar constant to that commonly used tomodel the sun. Assuming the following constants:d = 1.39e9 m=Diameter of the sunde = 1.27e7 m = Diameter of the earthRes = 1.49el1 m = Mean earth-to-sun distance (HINT: use this distance as the radius of asphere centered on the sun).

A blackbody is an ideal concept which irradiates every wavelength of light across the spectrum.…

Answered: 2. Can we Estimate the Solar Constant?…

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