The Solar Constant
- Since life on Earth is entirely dependant on the Sun’s energy, it is useful to quantify how much of its energy reaches the top of the atmosphere
- This is known as the solar constant
- The solar constant is defined as:
The amount of solar radiation across all wavelengths that is incident in one second on one square metre at the mean distance of the Earth from the Sun
- The value of the solar constant varies year-round because:
- The Earth’s is in an elliptical orbit around the Sun, meaning at certain times of year the Earth is closer to the Sun, and other times of year it is further away
- The Sun’s output varies by about 0.1% during its 11-year sunspot cycle
- Calculations of the solar constant assume that:
- This radiation is incident on a plane perpendicular to the Earth's surface
- The Earth is at its mean distance from the Sun
Worked example
The Sun emits 4 × 1026 J in one second. The mean distance of the Earth from the Sun is 1.5 × 1011 m.
Using this data, calculate the solar constant.
Step 1: List the known quantities
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- Power output of Sun, P = 4 × 1026 W
- Distance between the Earth and Sun, r = 1.5 × 1011 m
Step 2: Model the scenario using geometry
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- As light leaves the surface of the Sun, it begins to spread out uniformly through a spherical shell
- The surface area of a sphere = 4πr2
- The radius r of this sphere is equal to the distance between the Sun and the Earth
Step 3: Write an equation to calculate the solar constant
Solar constant =
Step 4: Calculate the solar constant
Solar constant = = 1415 W m–2
Solar constant = 1.4 kW m–2 (2 s.f)