Atmospheric effects have several impacts on the solar radiation at the Earth's surface. The major effects for photovoltaic applications are:
- a reduction in the power of the solar radiation due to absorption, scattering and reflection in the atmosphere;
- a change in the spectral content of the solar radiation due to greater absorption or scattering of some wavelengths;
- the introduction of a diffuse or indirect component into the solar radiation; and
- local variations in the atmosphere (such as water vapor, clouds and pollution) which have additional effects on the incident power, spectrum and directionality.
These effects are summarized in the figure below.
Absorption in the Atmosphere
As solar radiation passes through the atmosphere, gasses, dust and aerosols absorb the incident photons. Specific gasses, notably ozone (O3), carbon dioxide (CO2), and water vapor (H2O), have very high absorption of photons that have energies close to the bond energies of these atmospheric gases. This absorption yields deep troughs in the spectral radiation curve. For example, much of the far infrared light above 2 µm is absorbed by water vapor and carbon dioxide. Similarly, most of the ultraviolet light below 0.3 µm is absorbed by ozone (but not enough to completely prevent sunburn!).
While the absorption by specific gasses in the atmosphere change the spectral content of the terrestrial solar radiation, they have a relatively minor impact on the overall power. Instead, the major factor reducing the power from solar radiation is the absorption and scattering of light due to air molecules and dust. This absorption process does not produce the deep troughs in the spectral irradiance, but rather causes a power reduction dependent on the path length through the atmosphere. When the sun is overhead, the absorption due to these atmospheric elements causes a relatively uniform reduction across the visible spectrum, so the incident light appears white. However, for longer path lengths, higher energy (lower wavelength) light is more effectively absorbed and scattered. Hence in the morning and evening the sun appears much redder and has a lower intensity than in the middle of the day.
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The standard spectra given above and described in more detail in the appendices give a typical spectra for a sunlight. Computers models allow for more detailed models of the solar spectra for a particular location and time of day. The Simple Model of the Atmospheric Radiative Transfer of Sunshine, or SMARTS,3 is used to generate the standard solar spectra. The solar spectrum calculator at PV lighthouse also gives the solar spectrum as a function of location and time of the day. It uses a slightly simpler algorithm from Bird4
Direct and Diffuse Radiation Due to Scattering of Incident Light
Light is absorbed as it passes through the atmosphere and at the same time it is subject to scattering. One of the mechanisms for light scattering in the atmosphere is known as Rayleigh scattering which is caused by molecules in the atmosphere. Rayleigh scattering is particularly effective for short wavelength light (that is blue light) since it has a λ-4 dependence. In addition to Rayleigh scattering, aerosols and dust particles contribute to the scattering of incident light known as Mie scattering.
Effect of clouds and other local variations in the atmosphere
The final effect of the atmosphere on incident solar radiation is due to local variations in the atmosphere. Depending on the type of cloud cover, the incident power is severely reduced. An example of heavy cloud cover is shown below.
- 1. , Solar Cells: From Basic to Advanced Systems. New York: McGraw-Hill, 1983.
- 2. , Perception. New York: Alfred A. Knopf Inc, 1985.
- 3. , SMARTS2: a simple model of the atmospheric radiative transfer of sunshine: algorithms and performance assessment. Florida Solar Energy Center Cocoa, FL, 1995.
- 4. , “Simple Solar Spectral Model for Direct and Diffuse Irradiance on Horizontal and Tilted Planes at the Earth's Surface for Cloudless Atmospheres”, Journal of Climate and Applied Meteorology, vol. 25, no. 1, pp. 87 - 97, 1986.
- 5. , “Solar Power for Telecommunications”, The Telecommunication Journal of Australia, vol. 29, pp. 20-44, 1979.
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