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Solar
Luminosity (L) |
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the
constant flux of energy put out by the sun |
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L = 3.9 x 1026 W |
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Solar
Flux Density (Sd) |
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the
amount of solar energy per unit area on a sphere centered at the Sun with a
distance d |
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Sd = L / (4 p d2) W/m2 |
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Solar
energy incident on the Earth |
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= total amount of solar
energy can be absorbed by Earth |
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= (Solar constant) x (Shadow Area) |
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= S x p R2Earth |
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The
Earth warms up and has to emit radiative
energy back to the space to reach a equilibrium condition. |
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The
radiation emitted by the Earth is called “terrestrial radiation” which is
assumed to be like blackbody radiation. |
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