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Solar radiation is the radiation of the sun.

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Solar radiation is radiant energy emitted by the Sun, particularly electromagnetic energy. The spectrum of solar radiation is close to that one of a black body of the temperature T~5800 K. About half of the solar radiation is in the visible short-wave part of the electromagnetic spectrum. The other half is mostly in the near-Infrared part, with some in the ultraviolet part of the spectrum. The ultraviolet radiation not absorbed by the atmosphere or other protective coating is responsible for the change of color in skin pigments.

Solar radiation is commonly measured with a pyranometer or pyrheliometer.

Solar constant.

Solar radiation.
Solar irradiance spectrum at top of atmosphere.
Solar constant.
Solar constant 1978-2003 graph.
solar radiation.
A 1903 Langley bolograph with an erroneous solar constant of 2.54 calories.

The solar constant is the amount of incoming solar electromagnetic radiation per unit area, measured on the outer surface of Earth's atmosphere, in a plane perpendicular to the rays. The solar constant includes all types of solar radiation, not just the visible light. It is measured by satellite to be roughly 1366 watts per square meter, (although it fluctuates by a few parts per thousand from day to day and by about 6.9% during a year - from 1412 w/m2 in winter to 1321 w/m2 in summer). Thus, for the whole Earth, with a cross section of 127,400,000 km, the power is 1.7401017 W. The solar constant is not quite constant over long time periods; see solar variation.

The solar constant is relatively constant, but varies according to Sunspot activity. It affects mainly long-term climates, rather than short-term weather. The Earth receives a total amount of radiation determined by its cross section (p R2), but as the planet rotates this energy is distributed across the entire surface area (4 p R2). Hence, the average incoming solar radiation (known as "insolation") is one fourth the solar constant or ~342 W/m. At any given location and time, the amount received at the surface depends on the state of the atmosphere and the latitude.

The solar constant includes all wavelengths of solar electromagnetic radiation, not just the visible light. (See electromagnetic spectrum for more details) It is linked to the apparent magnitude of the Sun, -26.8, in that the solar constant and the magnitude of the sun are two methods of describing the apparent brightness of the Sun, though the magnitude only measures the visual output of the Sun.

In 1884 Samuel Pierpont Langley attempted to estimate the solar constant from Mount Whitney in California, and (by taking readings at different times of day) attempted to remove atmospheric absorption effects. However he obtained the incorrect value of 2903 W/m2, perhaps due to mathematical errors. Between 1902 and 1957, measurements by Charles Greeley Abbot and others at various high-altitude sites found values between 1322 and 1465 W/m2. Abbott proved that one of Langley's corrections was erroneously applied, and his results varied between 1.89 and 2.22 calories, and the variation appeared to be solar, not terrestrial.

The angular diameter of Earth seen from the sun is ca. 1/11,000 radian, so the solid angle of Earth seen from the sun is ca. 1/140,000,000 steradian. Thus, the sun emits about 2 billion times the amount of radiation that is caught by Earth, or about 3.861026 watts.

Climate effect of solar radiation: Solar dimming and insolation.

Solar irradiance spectrum.
Solar irradiance spectrum above atmosphere and at surface.

On Earth, solar radiation is obvious as daylight when the sun is above the horizon. This is during daytime, and also in summer near the poles at night, but not at all in winter near the poles. When the direct radiation is not blocked by clouds, it is experienced as sunshine, a combination of bright yellow light (sunlight in the strict sense) and heat. The heat on the body, on objects, etc., that is directly produced by the radiation should be distinguished from the increase in air temperature.

The amount of radiation intercepted by a planetary body varies as the square of the distance between the star and the planet. The Earth's orbit and obliquity change with time, sometimes achieving a nearly perfect circle, and at other times stretching out to an eccentricity of 5%. The total insolation remains almost constant but the seasonal and latitudinal distribution and intensity of solar radiation received at the Earth's surface also varies. For example, at latitudes of 65 degrees the change in solar energy in summer & winter can vary by more than 25% as a result of the Earth's orbital variation. Because changes in winter and summer tend to offset, the change in the annual average insolation at any given location is near zero, but the redistribution of energy between summer and winter does strongly affect the intensity of seasonal cycles. Such changes associated with the redistribution of solar energy are considered a likely cause for the coming and going of recent ice ages. (see: Milankovitch cycles).

The Sun
Image:Sun picture.png
Structure: Solar Core - Radiation Zone - Convection Zone
Atmosphere - Photosphere - Chromosphere - Transition region - corona
Extended Structure: Termination Shock - Heliosphere - Heliopause - Heliosheath - bow shock
Solar Phenomena: Sunspots - Faculae - Granules - Supergranulation - solar wind - Spicules
Coronal loops - Solar Flares - Solar Prominences - Coronal Mass Ejections
Moreton Waves - Coronal Holes
Other: Solar System - Solar Variation - Solar Dynamo - heliospheric current sheet - solar radiation - solar eclipse

Solar radiation extra pages.

Protecting from solar radiation.

One of the hazards of human spaceflight is the radiation damage of solar storms and cosmic rays. But it turns out the different parts of the human body are more susceptible to radiation than others. Although the best protection would be to get under cover, like in a spacecraft, future spacesuits could have extra radiation protection for specific areas of the body, like the hips (to prevent bone marrow damage).

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