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Energy Budget of the Earth-Atmosphere System. Energy Transfer. Conduction -- direct molecular transfer Convection -- fluids; air or water Sensible heat (temperature) Latent heat (evaporation/condensation) Radiation -- no transfer medium. Adiabatic Processes.
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Energy Transfer • Conduction -- direct molecular transfer • Convection -- fluids; air or water • Sensible heat (temperature) • Latent heat (evaporation/condensation) • Radiation -- no transfer medium
Global Energy Balance Inputs = Outputs
As the distance from the Sun increases, the intensity of the radiation diminishes in proportion to the distance squared (inverse square law). The solar constant is the amount of solar energy received by a surface perpendicular to the incoming rays at the mean Earth–Sun distance and is equal to 1367 W/m2.
Radiation Laws Stefan-Boltzmann Law E = sigma T (4th power) Wien's Law: Wavlength Max - inversely proportional to the temperature
Incoming solar radiation available is subject to a number of processes as it passes through the atmosphere. The clouds and gases of the atmosphere reflect 19 and 6 units, respectively, of insolation back to space. The atmosphere absorbs another 25 units. Only half of the insolation available at the top of the atmosphere actually reaches the surface, of which another 5 units are reflected back to space. The net solar radiation absorbed by the surface is 45 units.
