2. Can we Estimate the Solar Constant? A result from theoretical physics, known as the Stefan-Boltzmann law, states that the total power radiated by a blackbody at temperature T (K) per unit surface area is given by E=GT* where E is radiated power per unit surface area of the blackbody and o is the Stefan-Boltzmann constant equal to 5.67 x 10* Wm²K“. 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 solar energy [W/m] arriving at the top of Earth's atmosphere (we call that incident energy the solar constant). Compare your calculated estimate of the solar constant to that commonly used to model the sun. Assuming the following constants: d, = 1.39e9 m = Diameter of the sun de = 1.27e7 m = Diameter of the earth Res = 1.49el1 m = Mean earth-to-sun distance (HINT: use this distance as the radius of a sphere centered on the sun).

2. Can we Estimate the Solar Constant? A result from theoretical physics, known as the Stefan-Boltzmann law, states that the total power radiated by a blackbody at temperature T (K) per unit surface area is given by E=GT* where E is radiated power per unit surface area of the blackbody and o is the Stefan-Boltzmann constant equal to 5.67 x 10* Wm²K“. 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 solar energy [W/m] arriving at the top of Earth's atmosphere (we call that incident energy the solar constant). Compare your calculated estimate of the solar constant to that commonly used to model the sun. Assuming the following constants: d, = 1.39e9 m = Diameter of the sun de = 1.27e7 m = Diameter of the earth Res = 1.49el1 m = Mean earth-to-sun distance (HINT: use this distance as the radius of a sphere centered on the sun).