If you look at the center of the Sun,you see into the base of the photosphere at approximately 5800 K.If you look into the Sun nearer the edge,you might see as far as a layer above the base with a temperature of perhaps 5500 K.According to the Stefan-Boltzmann relation,what is the flux in the center of the solar disk compared to the flux near the edge?

Question

Quizplus · Accepted Answer

The Stefan-Boltzmann law states that the total energy emitted per unit area per unit time by a blackbody is proportional to the fourth power of its temperature. Mathematically, it can be written as:

F = σT^4

where F is the flux (energy per unit area per unit time), σ is the Stefan-Boltzmann constant, and T is the temperature.

Now, let's compare the flux at the center of the solar disk (T = 5800 K) to the flux near the edge (T = 5500 K):

F(center)/F(edge) = (σT(center)^4)/(σT(edge)^4)

F(center)/F(edge) = (5800/5500)^4

F(center)/F(edge) = 1.242

Therefore, the flux at the center of the solar disk is about 1.24 times higher than the flux near the edge.

The correct answer is D.

If You Look at the Center of the Sun,you See