Solar constant

The solar constant (denoted as S☉ by the IAU standard) is a mathematical equation averaging the amount of energy received by a given area one astronomical unit away from the Sun. To put simply, it is measuring the amount of energy the Sun is giving Earth. More specifically, it is a flux density measuring mean solar electromagnetic radiation (total solar irradiance) per unit area. It is measured on a surface perpendicular to the rays, one astronomical unit (au) from the Sun (roughly the distance from the Sun to the Earth).

The solar constant includes radiation over the entire electromagnetic spectrum. It is measured by satellite as being 1.361 kilowatts per square meter (kW/m2) at solar minimum (the time in the 11-year solar cycle when the number of sunspots is minimal) and approximately 0.1% greater (roughly 1.362 kW/m2) at solar maximum.

The solar "constant" is not a physical constant in the modern CODATA scientific sense; that is, it is not like the Planck constant or the speed of light which are absolutely constant in physics. The solar constant is an average of a varying value. In the past 400 years it has varied less than 0.2 percent. Billions of years ago, it was significantly lower. This is important because the amount of sunlight we receive affects atmospheric and oceanic processes.

This constant is used in the calculation of radiation pressure, which aids in the calculation of a force on a solar sail.

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