(Heat transfer) Radiation is the transfer of heat via electromagnetic wave propagation. Ex...

(Heat transfer) Radiation is the transfer of heat via electromagnetic wave propagation. Examples of heat transfer are the heat radiated from the sun, the heat radiated from Earth, and the heat given off in the evening by objects, such as cars and brick walls, warmed by the sun during the day. The heat radiated by an object can be calculated by using Stefan-Boltzmann’s Law:

E = e × σ × T4

E is the energy radiated per second per square meter of its surface.

e is the emissivity of the substance (a number between 0 and 1).

σ is Stefan-Boltzmann’s constant (5.6697 . 10-8 watts/m2K4).

T is the surface temperature in degrees Kelvin (°K = °C + 273). 

An ideal radiator, such as the sun, has an emissivity of 1, and the heat generated from the sun, with a surface temperature of approximately 6000°K, is as follows:

E = 5.6697 . 10-8 watts/m2K4 (6 . 103K)4

    = 5.6697 . 10-8 watts/m2K4 (1296 . 1012K4) = 7.3 . 107 watts/m2

    = 73,000,000 watts/m2

Using the formula and this information, write a C++ program that accepts a planet’s temperature (assuming an emissivity of 1) and provides the heat generated from the planet as its output. After determining that your program is working correctly (make sure it produces the correct radiation for the sun), use it to complete the following chart (make sure to use correct units):