Introduction:
The solar constant represents the amount of solar electromagnetic radiation received at the outer atmosphere of the Earth. It is a measure of the Sun's power output and is an essential factor in the Earth's climate and energy balance. Any change in the temperature of the Sun would affect the solar constant.

Impact of Decreased Temperature:
If the temperature of the Sun were to decrease by 60K, it would result in a decrease in its power output. This decrease in power output would directly impact the solar constant, causing it to change.

Calculation of Solar Constant:
The solar constant, denoted by "S", is calculated by dividing the Sun's total power output by the surface area of a sphere with a radius equal to the average distance between the Earth and the Sun. The value of the solar constant is approximately 1361 Watts per square meter.

Explanation of Change in Solar Constant:
When the temperature of the Sun decreases, its power output decreases as well. This reduction in power output is due to the fact that the Sun's energy generation is primarily dependent on thermonuclear reactions occurring in its core. A decrease in temperature would result in a decrease in the rate of these reactions, leading to a decrease in power output.

As a result, the solar constant would also decrease. The reduced power output of the Sun means that less electromagnetic radiation reaches the outer atmosphere of the Earth, resulting in a decrease in the solar constant value.

Quantifying the Change:
The exact change in the solar constant due to a 60K decrease in the Sun's temperature can be calculated using the Stefan-Boltzmann law. This law relates the temperature of a black body (like the Sun) to its radiant power output. According to the law, the power output of a black body is proportional to the fourth power of its absolute temperature.

By applying this law, we can calculate the change in power output and subsequently the change in the solar constant. However, the exact value of the change cannot be determined without knowing the initial temperature of the Sun.

Conclusion:
In summary, if the temperature of the Sun were to decrease by 60K, the solar constant would also decrease. This change is a result of the reduced power output of the Sun, which directly affects the amount of solar electromagnetic radiation reaching the Earth's outer atmosphere. The exact quantification of this change requires knowledge of the initial temperature of the Sun and the application of the Stefan-Boltzmann law.

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