The solar constant is the amount of solar radiation that reaches the Earth's upper atmosphere. It is a measure of the amount of energy that the Earth receives from the Sun. Any change in the temperature of the Sun will affect the solar constant.


If the temperature of the Sun is decreased by 1%, it will result in a decrease in the energy output of the Sun. According to the Stefan-Boltzmann law, the energy output of a black body is proportional to the fourth power of its temperature. Therefore, a 1% decrease in the temperature of the Sun will result in a decrease in its energy output by approximately:

(1% / 100%) x (4 / 1) = 0.04 or 4%

This means that if the temperature of the Sun is decreased by 1%, the solar constant will decrease by approximately 4%.


In conclusion, any change in the temperature of the Sun will affect the solar constant. A 1% decrease in the temperature of the Sun will result in a decrease in the solar constant by approximately 4%.