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Week 1 - introduction to the climate system (E3
and G1, 2, 5)
subcomponents
global energy cycle
global water cycle |
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Week 2 - atmosphere (E4 and G6)
general circulation
jetstream and midlatitude storm
tropical trade winds and monsoons |
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Week 3 - ocean (E5 and G7)
wind-driven circulation
thermohaline circulations
meridional heat transport |
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Week 4 - land surface (G5)
energy, water, and heat properties |
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Week 5 - climate sensitivity and feedback
mechanisms (G9)
measurement of sensitivity
cloud-radiation feedback
ice-albedo feedback
water vapor feedback |
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*** MID-TERM*** |
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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
Constant (S) |
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The
solar energy density at the mean distance of Earth from the sun (1.5
x 1011 m) |
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S
= L / (4 p d2) |
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= (3.9 x 1026 W) / [4 x 3.14 x (1.5 x 1011 m)2] |
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= 1370 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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Blackbody |
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A
blackbody is something that emits (or absorbs) electromagnetic radiation
with 100% efficiency at all wavelength. |
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Blackbody Radiation |
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The
amount of the radiation emitted by a blackbody depends on the absolute
temperature of the blackbody. |
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The
Planck function relates the intensity of radiation from a blackbody to its
wavelength. |
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Notes