Solar constant

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Solar irradiance spectrum at top of atmosphere, on a linear scale and plotted against wavenumber.

The solar constant, a measure of flux density, is the amount of incoming solar electromagnetic radiation (the solar irradiance) per unit area that would be incident on a plane perpendicular to the rays, at a distance of one astronomical unit (AU) (roughly the mean distance from the Sun to the Earth). The solar constant includes all types of solar radiation, not just the visible light. It is measured by satellite to be roughly 1.361 kilowatts per square meter (kW/m²) at solar minimum and approximately 0.1% greater (roughly 1.362 kW/m²) at solar maximum.[1]

Calculation[edit]

Solar irradiance is measured by satellite near the outer surface of Earth's atmosphere,[2] and is then adjusted using the inverse square law to infer the magnitude of solar irradiance at one AU and find the solar constant.[3] The approximate average value cited,[1] 1.361 kW/m², which is 81.66 kJ/m² per minute in SI units, is equivalent to approximately 1.952 calories per minute per square centimeter, or 1.952 langleys.

Solar output is nearly, but not quite, constant. Variations in total solar irradiance were too small to detect with technology available before the satellite era. Total solar output is now measured as varying (over the last three 11-year sunspot cycles) by approximately 0.1%;[4] see solar variation for details.

Historical measurements[edit]

In 1838, Claude Pouillet made the first estimate of the solar constant. Using a very simple pyrheliometer he developed, he obtained a value of 1228 W/m²,[5] very close to the current estimate.

In 1875, Jules Violle resumed the work of Pouillet and offered a somewhat larger estimate of 1.7 kW/m² based, in part, on a celebrated measurement that he made from Mont Blanc in France.

In 1884, Samuel Pierpont Langley attempted to estimate the solar constant from Mount Whitney in California. By taking readings at different times of day, he tried to correct for effects due to atmospheric absorption. However, the final value he proposed, 2.903 kW/m², was much too large.

A 1903 Langley bolograph with an erroneous solar constant of 2.54 calories/minute/square centimeter.

Between 1902 and 1957, measurements by Charles Greeley Abbot and others at various high-altitude sites found values between 1.322 and 1.465 kW/m². Abbot showed that one of Langley's corrections was erroneously applied. Abbot's results varied between 1.89 and 2.22 calories (1.318 to 1.548  kW/m²), a variation that appeared to be due to the Sun and not the Earth's atmosphere.[6]

Relationship to other measurements[edit]

Solar irradiance[edit]

The actual direct solar irradiance at the top of the atmosphere fluctuates by about 6.9% during a year (from 1.412 kW/m² in early January to 1.321 kW/m² in early July) due to the Earth's varying distance from the Sun, and typically by much less than 0.1% from day to day. Thus, for the whole Earth (which has a cross section of 127,400,000 km²), the power is 1.740×1017 W, plus or minus 3.5%. The solar constant does not remain constant over long periods of time (see Solar variation), but over a year the solar constant varies much less than the solar irradiance measured at the top of the atmosphere. This is because the solar constant is measured at a fixed distance of 1 AU while the solar irradiance will be affected by the ellipticity of the Earth's orbit.

The Earth receives a total amount of radiation determined by its cross section (π·RE²), but as it rotates this energy is distributed across the entire surface area (4·π·RE²). Hence the average incoming solar radiation, taking into account the angle at which the rays strike and that at any one moment half the planet does not receive any solar radiation, is one-fourth the solar constant (approximately 340 W/m²). At any given moment, the amount of solar radiation received at a location on the Earth's surface depends on the state of the atmosphere, the location's latitude, and the time of day.

Apparent magnitude[edit]

The solar constant includes all wavelengths of solar electromagnetic radiation, not just the visible light (see Electromagnetic spectrum). It is positively correlated with the apparent magnitude of the Sun which is −26.8. The solar constant and the magnitude of the Sun are two methods of describing the apparent brightness of the Sun, though the magnitude is based on the Sun's visual output only.

The Sun's total radiation[edit]

The angular diameter of the Earth as seen from the Sun is approximately 1/11,700 radians (about 18 arc-seconds), meaning the solid angle of the Earth as seen from the Sun is approximately 1/175,000,000 of a steradian. Thus the Sun emits about 2.2 billion times the amount of radiation that is caught by Earth, in other words about 3.86×1026 watts.[7]

Past variations in solar irradiance[edit]

Space-based observations of solar irradiance started in 1978. These measurements show that the solar constant is not constant. It varies with the 11-year sunspot solar cycle. When going further back in time, one has to rely on irradiance reconstructions, using sunspots for the past 400 years or cosmogenic radionuclides for going back 10,000 years. Such reconstructions show that solar irradiance varies with distinct periodicities. These cycles are: 11 years (Schwabe), 88 years (Gleisberg cycle), 208 years (DeVries cycle) and 1,000 years (Eddy cycle).[8][9][10][11][12]

See also[edit]

References[edit]

  1. ^ a b Kopp, G.; Lean, J. L. (2011). "A new, lower value of total solar irradiance: Evidence and climate significance" (PDF). Geophysical Research Letters 38: n/a. Bibcode:2011GeoRL..38.1706K. doi:10.1029/2010GL045777.  edit
  2. ^ Satellite observations of total solar irradiance
  3. ^ http://www.ngdc.noaa.gov/stp/SOLAR/ftpsolarirradiance.html
  4. ^ Willson, Richard C.; H.S. Hudson (1991). "The Sun's luminosity over a complete solar cycle". Nature 351 (6321): 42–4. Bibcode:1991Natur.351...42W. doi:10.1038/351042a0. 
  5. ^ The measurement of the solar constant by Claude Pouillet, by J-L Dufresne, La Météorologie, No. 60, pp. 36-43, Feb. 2008.
  6. ^ Public Domain One or more of the preceding sentences incorporates text from a publication now in the public domainChisholm, Hugh, ed. (1911). "Sun". Encyclopædia Britannica (11th ed.). Cambridge University Press. 
  7. ^ The Sun at nine planets.org
  8. ^ Wang et al.(2005), The Astrophysical Journal, Volume 625, Issue 1, Pages 522-538, http://dx.doi.org/10.1086/429689
  9. ^ Steinhilber et al.(2009), Geophysical Research Letters, Volume 36, L19704, http://dx.doi.org/10.1051/0004-6361/200811446
  10. ^ Vieira et al.(2011), Astronomy&Astrophysics, Volume 531, A6, http://dx.doi.org/10.1051/0004-6361/201015843
  11. ^ Steinhilber et al.(2012), Proceedings of the National Academy of Sciences, Early Edition http://dx.doi.org/10.1073/pnas.1118965109
  12. ^ Vieira, L. E. A., A. Norton, T. Dudok de Wit, M. Kretzschmar, G. A. Schmidt, and M. C. M. Cheung (2012), How the inclination of Earth's orbit affects incoming solar irradiance, Geophys. Res. Lett., 39, L16104, doi:10.1029/2012GL052950