Sunlight

"Sunshine" redirects here. For other uses, see Sunshine (disambiguation).
For natural lighting of interior spaces by admitting sunlight, see Daylighting. For solar energy available from sunlight, see Insolation. For other uses, see Sunlight (disambiguation).
Sunlight shining through clouds, giving rise to crepuscular rays

Sunlight is a portion of the electromagnetic radiation given off by the Sun, in particular infrared, visible, and ultraviolet light. On Earth, sunlight is filtered through Earth's atmosphere, and is obvious as daylight when the Sun is above the horizon. When the direct solar radiation is not blocked by clouds, it is experienced as sunshine, a combination of bright light and radiant heat. When it is blocked by the clouds or reflects off other objects, it is experienced as diffused light. The World Meteorological Organization uses the term "sunshine duration" to mean the cumulative time during which an area receives direct irradiance from the Sun of at least 120 watts per square meter.[1]

The ultraviolet radiation in sunlight has both positive and negative health effects, as it is both a principal source of vitamin D3 and a mutagen.

Summary

Researchers may record sunlight using a sunshine recorder, pyranometer, or pyrheliometer.

Sunlight takes about 8.3 minutes to reach Earth from the surface of the Sun. A photon starting at the centre of the Sun and changing direction every time it encounters a charged particle would take between 10,000 and 170,000 years to get to the surface.[2]

The total amount of energy received at ground level from the Sun at the zenith depends on the distance to the Sun and thus on the time of year. It is about 3.3% higher than average in January and 3.3% lower in July (see below). If the extraterrestrial solar radiation is 1367 watts per square meter (the value when the Earth–Sun distance is 1 astronomical unit), then the direct sunlight at Earth's surface when the Sun is at the zenith is about 1050 W/m2, but the total amount (direct and indirect from the atmosphere) hitting the ground is around 1120 W/m2.[3] In terms of energy, sunlight at Earth's surface is around 52 to 55 percent infrared (above 700 nm), 42 to 43 percent visible (400 to 700 nm), and 3 to 5 percent ultraviolet (below 400 nm).[4] At the top of the atmosphere, sunlight is about 30% more intense, having about 8% ultraviolet (UV),[5] with most of the extra UV consisting of biologically damaging short-wave ultraviolet.[6]

Direct sunlight has a luminous efficacy of about 93 lumens per watt of radiant flux, higher than most artificial lighting, including fluorescent. Multiplying the figure of 1050 watts per square metre by 93 lumens per watt indicates that bright sunlight provides an illuminance of approximately 98 000 lux (lumens per square meter) on a perpendicular surface at sea level. The illumination of a horizontal surface will be considerably less than this if the Sun is not very high in the sky. Averaged over a day, the highest amount of sunlight on a horizontal surface occurs in January at the South Pole (see insolation).

Sunlight is a key factor in photosynthesis, the process used by plants and other autotrophic organisms to convert light energy, normally from the Sun, into chemical energy that can be used to fuel the organisms' activities.

Composition and power

Solar irradiance spectrum above atmosphere and at surface. Extreme UV and X-rays are produced (at left of wavelength range shown) but comprise very small amounts of the Sun's total output power.
This spectrum, created at the McMath-Pierce Solar Observatory, shows that the Sun emits light of nearly every color, but is brightest in yellow-green light. The dark patches in the spectrum arise from gas at or above the Sun's surface absorbing light. Because different types of gas absorb different colors of light, it is possible to determine which gases are present in the Sun's photosphere. Helium, for example, was first discovered in 1870 by analyzing the solar spectrum and was only later found on Earth.
See also: Ultraviolet, Infrared and Light

The spectrum of the Sun's solar radiation is close to that of a black body[7][8] with a temperature of about 5,800 K.[9] The Sun emits EM radiation across most of the electromagnetic spectrum. Although the Sun produces Gamma rays as a result of the nuclear fusion process, these super-high-energy photons are converted by internal absorption and thermalization to lower-energy photons before they reach the Sun's surface and are emitted out into space. As a result, the Sun does not emit gamma rays, from this process, although it does produce gamma rays from solar flares.[10] The Sun does also emit X-rays, ultraviolet, visible light, infrared, and even radio waves;[11] the only direct signature of the nuclear process is the emission of neutrinos.

Although the solar corona is a source of extreme ultraviolet and X-ray radiation, these rays make up only a very small amount of the power output of the Sun (see spectrum at right). The spectrum of nearly all solar electromagnetic radiation striking the Earth's atmosphere spans a range of 100 nm to about 1 mm (1,000,000 nm). This band of significant radiation power can be divided into five regions in increasing order of wavelengths:[12]

Published tables

Tables of direct solar radiation on various slopes from 0 to 60 degrees North Latitude, in calories per square centimetre, issued in 1972 and published by Pacific Northwest Forest and Range Experiment Station|Forest Service, U.S. Department of Agriculture, Portland, Oregon, USA, are available on the web.[14]

Calculation

To calculate the amount of sunlight reaching the ground, both Earth's elliptical orbit and the attenuation by Earth's atmosphere have to be taken into account. The extraterrestrial solar illuminance (Eext), corrected for the elliptical orbit by using the day number of the year (dn), is given to a good approximation by[15]

E_{\rm ext}= E_{\rm sc} \cdot \left(1+0.033412 \cdot \cos\left(2\pi\frac{{\rm dn}-3}{365}\right)\right),

where dn=1 on January 1; dn=2 on January 2; dn=32 on February 1, etc. In this formula dn-3 is used, because in modern times Earth's perihelion, the closest approach to the Sun and, therefore, the maximum Eext occurs around January 3 each year. The value of 0.033412 is determined knowing that the ratio between the perihelion (0.98328989 AU) squared and the aphelion (1.01671033 AU) squared should be approximately 0.935338.

The solar illuminance constant (Esc), is equal to 128×103 lx. The direct normal illuminance (Edn), corrected for the attenuating effects of the atmosphere is given by:

E_{\rm dn}=E_{\rm ext}\,e^{-cm},

where c is the atmospheric extinction and m is the relative optical airmass. The atmospheric extinction brings the number of lux down to around 100 000.

Solar constant

Main article: Solar constant
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 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 Earth). The "solar constant" includes all types of solar radiation, not just the visible light. Its average value was thought to be approximately 1.366 kW/m²,[16] varying slightly with solar activity, but recent recalibrations of the relevant satellite observations indicate a value closer to 1.361 kW/m² is more realistic.[17]

Total (TSI) and spectral solar irradiance (SSI) upon Earth

Total Solar Irradiance (TSI) – the amount of solar radiation received at the top of Earth's atmosphere – has been measured since 1978 by series of overlapping NASA and ESA satellite experiments to be 1.361 kilo⁠watts per square meter (kW/m²).[16][18][19][20] TSI observations are continuing today with the ACRIMSAT/ACRIM3, SOHO/VIRGO and SORCE/TIM satellite experiments.[21] Variation of TSI has been discovered on many timescales including the solar magnetic cycle [22] and many shorter periodic cycles.[23] TSI provides the energy that drives Earth's climate, so continuation of the TSI time series database is critical to understanding the role of solar variability in climate change.

Spectral Solar Irradiance (SSI) - the spectral distribution of the TSI - has been monitored since 2003 by the SORCE Spectral Irradiance Monitor (SIM). It has been found that SSI at UV (ultraviolet) wavelength corresponds in a less clear, and probably more complicated fashion, with Earth's climate responses than earlier assumed, fueling broad avenues of new research in “the connection of the Sun and stratosphere, troposphere, biosphere, ocean, and Earth’s climate”.[24]

Intensity in the Solar System

Sunlight on Mars is dimmer than on Earth. This photo of a Martian sunset was imaged by Mars Pathfinder.

Different bodies of the Solar System receive light of an intensity inversely proportional to the square of their distance from Sun. A rough table comparing the amount of solar radiation received by each planet in the Solar System follows (from data in ):

Planet or dwarf planet distance (AU) Solar radiation (W/m²)
PerihelionAphelion maximumminimum
Mercury  0.3075  0.4667 14,446  6,272
Venus  0.7184  0.7282  2,647  2,576
Earth  0.9833  1.017  1,413  1,321
Mars  1.382  1.666    715    492
Jupiter  4.950  5.458     55.8     45.9
Saturn  9.048 10.12     16.7     13.4
Uranus 18.38 20.08      4.04      3.39
Neptune 29.77 30.44      1.54      1.47
Pluto29.6648.87      1.55      0.57

The actual brightness of sunlight that would be observed at the surface depends also on the presence and composition of an atmosphere. For example, Venus's thick atmosphere reflects more than 60% of the solar light it receives. The actual illumination of the surface is about 14,000 lux, comparable to that on Earth "in the daytime with overcast clouds".[25]

Sunlight on Mars would be more or less like daylight on Earth wearing sunglasses, and, as can be seen in the pictures taken by the rovers, there is enough diffuse sky radiation that shadows would not seem particularly dark. Thus, it would give perceptions and "feel" very much like Earth daylight.

For comparison purposes, sunlight on Saturn is slightly brighter than Earth sunlight at the average sunset or sunrise (see daylight for comparison table). Even on Pluto the sunlight would still be bright enough to almost match the average living room. To see sunlight as dim as full moonlight on Earth, a distance of about 500 AU (~69 light-hours) is needed; there are only a handful of objects in the Solar System known to orbit farther than such a distance, among them 90377 Sedna and (87269) 2000 OO67.

Surface illumination

The spectrum of surface illumination depends upon solar elevation due to atmospheric effects, with the blue spectral component dominating during twilight before and after sunrise and sunset, respectively, and red dominating during sunrise and sunset. These effects are apparent in natural light photography where the principal source of illumination is sunlight as mediated by the atmosphere.

While the color of the sky is usually determined by Rayleigh scattering, an exception occurs at sunset and twilight. "Preferential absorption of sunlight by ozone over long horizon paths gives the zenith sky its blueness when the sun is near the horizon".[26]

See diffuse sky radiation for more details.

Spectral composition of surface illumination

The Sun's electromagnetic radiation which illuminates Earth's surface is predominantly light that falls within the range of wavelengths to which the visual systems of the animals that inhabit Earth's surface are sensitive. The Sun may therefore be said to illuminate, which is a measure of the light within a specific sensitivity range. Many animals (including humans) have a sensitivity range of approximately 400–700 nm,[27] and given optimal conditions the absorption and scattering by Earth's atmosphere produces illumination that approximates an equal-energy illuminant for most of this range. The useful range for color vision in humans, for example, is approximately 450–650 nm. Aside from effects that arise at sunset and sunrise, the spectral composition changes primarily in respect to how directly sunlight is able to illuminate. When illumination is indirect, Rayleigh scattering in the upper atmosphere will lead blue wavelengths to dominate. Water vapour in the lower atmosphere produces further scattering and ozone, dust and water particles will also absorb selective wavelengths.[28][29]

Spectrum of the visible wavelengths at approximately sea level; illumination by direct sunlight compared with direct sunlight scattered by cloud cover and with indirect sunlight by varying degrees of cloud cover. The yellow line shows the spectrum of direct illumination under optimal conditions. The other illumination conditions are scaled to show their relation to direct illumination. The units of spectral power are simply raw sensor values (with a linear response at specific wavelengths).

Climate effects

Further information: Solar variation, Solar dimming, Insolation and Sunshine duration

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, combining the perception of bright white light (sunlight in the strict sense) and warming. The warming on the body, the ground, and other objects depends on the absorption of the electromagnetic radiation in the form of heat.

The amount of radiation intercepted by a planetary body varies inversely with the square of the distance between the star and the planet. Earth's orbit and obliquity change with time (over thousands of years), sometimes forming a nearly perfect circle, and at other times stretching out to an orbital eccentricity of 5% (currently 1.67%). As the orbit changes, the total insolation over a year remains almost constant due to Kepler's second law,

\tfrac{2A}{r^2}dt = d\theta,

where A is the "areal velocity" invariant. That is, the integration over the orbital period (also invariant) is a constant.

\int_{0}^{T} \tfrac{2A}{r^2}dt = \int_{0}^{2\pi} d\theta = \mathrm{constant}.

If we assume the solar radiation power P as a constant over time and the solar irradiation given by the inverse-square law, we obtain also the average insolation as a constant.

But the seasonal and latitudinal distribution and intensity of solar radiation received at Earth's surface also varies.[30] For example, at latitudes of 65 degrees, the change in solar energy in summer and winter can vary by more than 25% as a result of 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).

Past variations in solar irradiance

Space-based observations of solar irradiance started in 1978. These measurements show that the solar constant is not constant. It varies on many periodic cycles including the 11-year sunspot solar cycle.[22] 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 have been done.[31][32][33][34] These studies show that solar irradiance does vary with distinct periodicities such as: 11 years (Schwabe), 88 years (Gleisberg cycle), 208 years (DeVries cycle) and 1,000 years (Eddy cycle).

Life on Earth

The existence of nearly all life on Earth is fueled by light from the Sun. Most autotrophs, such as plants, use the energy of sunlight, combined with carbon dioxide and water, to produce simple sugars—a process known as photosynthesis. These sugars are then used as building-blocks and in other synthetic pathways that allow the organism to grow.

Heterotrophs, such as animals, use light from the Sun indirectly by consuming the products of autotrophs, either by consuming autotrophs, by consuming their products, or by consuming other heterotrophs. The sugars and other molecular components produced by the autotrophs are then broken down, releasing stored solar energy, and giving the heterotroph the energy required for survival. This process is known as cellular respiration.

In prehistory, humans began to further extend this process by putting plant and animal materials to other uses. They used animal skins for warmth, for example, or wooden weapons to hunt. These skills allowed humans to harvest more of the sunlight than was possible through glycolysis alone, and human population began to grow.

During the Neolithic Revolution, the domestication of plants and animals further increased human access to solar energy. Fields devoted to crops were enriched by inedible plant matter, providing sugars and nutrients for future harvests. Animals that had previously provided humans with only meat and tools once they were killed were now used for labour throughout their lives, fueled by grasses inedible to humans.

The more recent discoveries of coal, petroleum and natural gas are modern extensions of this trend. These fossil fuels are the remnants of ancient plant and animal matter, formed using energy from sunlight and then trapped within Earth for millions of years. Because the stored energy in these fossil fuels has accumulated over many millions of years, they have allowed modern humans to massively increase the production and consumption of primary energy. As the amount of fossil fuel is large but finite, this cannot continue indefinitely, and various theories exist as to what will follow this stage of human civilization (e.g., alternative fuels, Malthusian catastrophe, new urbanism, peak oil).

Cultural aspects

Claude Monet: Le déjeuner sur l'herbe

The effect of sunlight is relevant to painting, evidenced for instance in works of Claude Monet on outdoor scenes and landscapes.

Winter sunshine

Many people find direct sunlight to be too bright for comfort, especially when reading from white paper upon which the sun is directly shining. Indeed, looking directly at the sun can cause long-term vision damage. To compensate for the brightness of sunlight, many people wear sunglasses. Cars, many helmets and caps are equipped with visors to block the sun from direct vision when the sun is at a low angle. Sunshine is often blocked from entering buildings through the use of walls, window blinds, awnings, shutters, curtains, or nearby shade trees.

In colder countries, many people prefer sunnier days and often avoid the shade. In hotter countries, the converse is true; during the midday hours, many people prefer to stay inside to remain cool. If they do go outside, they seek shade that may be provided by trees, parasols, and so on.

In Hinduism the sun is considered to be a god as it is the source of life and energy on earth.

Sunbathing

Main article: Sun tanning

Sunbathing is a popular leisure activity in which a person sits or lies in direct sunshine. People often sunbathe in comfortable places where there is ample sunlight. Some common places for sunbathing include beaches, open air swimming pools, parks, gardens, and sidewalk cafes. Sunbathers typically wear limited amounts of clothing or some simply go nude. For some, an alternative to sunbathing is the use of a sunbed that generates ultraviolet light and can be used indoors regardless of weather conditions. Tanning beds have been banned in a number of states in the world.

For many people with light skin, one purpose for sunbathing is to darken one's skin color (get a sun tan), as this is considered in some cultures to be attractive, associated with outdoor activity, vacations/holidays, and health. Some people prefer naked sunbathing so that an "all-over" or "even" tan can be obtained, sometimes as part of a specific lifestyle.

For people suffering from psoriasis, sunbathing is an effective way of healing the symptoms.

Skin tanning is achieved by an increase in the dark pigment inside skin cells called melanocytes, and is an automatic response mechanism of the body to sufficient exposure to ultraviolet radiation from the sun or from artificial sunlamps. Thus, the tan gradually disappears with time, when one is no longer exposed to these sources.

Effects on human health

The ultraviolet radiation in sunlight has both positive and negative health effects, as it is both a principal source of vitamin D3 and a mutagen.[35] A dietary supplement can supply vitamin D without this mutagenic effect,[36] but bypasses natural mechanisms that would prevent overdoses of vitamin D generated internally from sunlight. Vitamin D has a wide range of positive health effects, which include strengthening bones[37] and possibly inhibiting the growth of some cancers.[38][39] Sun exposure has also been associated with the timing of melatonin synthesis, maintenance of normal circadian rhythms, and reduced risk of seasonal affective disorder.[40]

Long-term sunlight exposure is known to be associated with the development of skin cancer, skin aging, immune suppression, and eye diseases such as cataracts and macular degeneration.[41] Short-term overexposure is the cause of sunburn, snow blindness, and solar retinopathy.

UV rays, and therefore sunlight and sunlamps, are the only listed carcinogens that are known to have health benefits,[42] and a number of public health organizations state that there needs to be a balance between the risks of having too much sunlight or too little.[43] There is a general consensus that sunburn should always be avoided.

See also

References

  1. ↑ "Chapter 8 – Measurement of sunshine duration" (PDF). CIMO Guide. World Meteorological Organization. Retrieved 2008-12-01.
  2. ↑ "NASA: The 8-minute travel time to Earth by sunlight hides a thousand-year journey that actually began in the core". NASA, sunearthday.nasa.gov. Retrieved 2012-02-12.
  3. ↑ "Introduction to Solar Radiation". Newport Corporation. Archived from the original on Oct 29, 2013.
  4. ↑ Calculated from data in "Reference Solar Spectral Irradiance: Air Mass 1.5". National Renewable Energy Laboratory. Archived from the original on Sep 28, 2013. Retrieved 2009-11-12. The first of each set of two figures is for total solar radiation reaching a panel aimed at the Sun (which is 42° above the horizon), whereas the second figure of each pair is the "direct plus circumsolar" radiation (circumsolar meaning coming from the part of the sky within a couple degrees of the Sun). The totals, from 280 to 4000 nm, are 1000.4 and 900.1 W/m2 respectively. It would be good to have more direct figures from a good source, rather than summing thousands of numbers in a database.
  5. ↑ Calculated from the ASTM spectrum cited above.
  6. ↑ Qiang, Fu (2003). "Radiation (Solar)" (PDF). In Holton, James R. Encyclopedia of atmospheric sciences 5. Amsterdam: Academic Press. pp. 1859–1863. ISBN 978-0-12-227095-6. OCLC 249246073.
  7. ↑ Appleton, E. V., Nature 3966:535 (1945)
  8. ↑ Iqbal, M., "An Introduction to Solar Radiation", Academic Press (1983), Chap. 3
  9. ↑ NASA Solar System Exploration - Sun: Facts & Figures retrieved 27 April 2011 "Effective Temperature ... 5777 K"
  10. ↑ http://www.nasa.gov/mission_pages/GLAST/news/highest-energy.html
  11. ↑ "The Multispectral Sun, from the National Earth Science Teachers Association". Windows2universe.org. 2007-04-18. Retrieved 2012-02-12.
  12. ↑ Naylor, Mark; Kevin C. Farmer (1995). "Sun damage and prevention". Electronic Textbook of Dermatology. The Internet Dermatology Society. Retrieved 2008-06-02.
  13. ↑ tanning booth cancer
  14. ↑ John Buffo; Leo J. Fritschen; James L. Murphy (1972). "Direct Solar Radiation On Various Slopes From 0 To 60 Degrees North Latitude" (PDF). Pacific Northwest Forest and Range Experiment Station, Forest Service, U.S. Department of Agriculture, Portland, Oregon,USA. Retrieved 15 Jan 2014.
  15. ↑ C. KANDILLI & K. ULGEN. "Solar Illumination and Estimating Daylight Availability of Global Solar Irradiance". Energy Sources.
  16. ↑ 16.0 16.1 "Satellite observations of total solar irradiance". Acrim.com. Retrieved 2012-02-12.
  17. ↑ G. Kopp, Greg; J. Lean (2011). "A new, lower value of total solar irradiance: Evidence and climate significance". Geophys. Res. Lett. 38: L01706. Bibcode:2011GeoRL..3801706K. doi:10.1029/2010GL045777.
  18. ↑ Willson, R. C., and A. V. Mordvinov (2003), Secular total solar irradiance trend during solar cycles 21–23, Geophys. Res. Lett., 30(5), 1199, doi:10.1029/2002GL016038 ACRIM
  19. ↑ "Construction of a Composite Total Solar Irradiance (TSI) Time Series from 1978 to present". Retrieved 2005-10-05.
  20. ↑ Current Projects
  21. ↑ Graphics Gallery
  22. ↑ 22.0 22.1 "Graphics Gallery". Acrim.com. Retrieved 2014-04-21.
  23. ↑ http://www.acrim.com/Comparison%20of%20TSI%20Results.htm
  24. ↑ "NASA Goddard Space Flight Center: Solar Radiation". Atmospheres.gsfc.nasa.gov. 2012-02-08. Retrieved 2012-02-12.
  25. ↑ "The Unveiling of Venus: Hot and Stifling". Science News 109 (25): 388. 1976-06-19. doi:10.2307/3960800. JSTOR 3960800. 100 watts per square meter ... 14,000 lux ... corresponds to ... daytime with overcast clouds
  26. ↑ Craig Bohren. "Atmospheric Optics" (PDF).
  27. ↑ Buser, Pierre A.; Imbert, Michel (1992). Vision. MIT Press. p. 50. ISBN 978-0-262-02336-8. Retrieved 11 October 2013. Light is a special class of radiant energy embracing wavelengths between 400 and 700 nm (or mμ), or 4000 to 7000 Å.
  28. ↑ Wyszecki, Günter; Stiles, W. S. (1967). Color Science: Concepts and Methods, Quantitative Data and Formulas. John Wiley & Sons. p. 8.
  29. ↑ MacAdam, David L. (1985). Color Measurement: Theme and Variations (Second Revised ed.). Springer. pp. 33–35. ISBN 0-387-15573-2.
  30. ↑ "Graph of variation of seasonal and latitudinal distribution of solar radiation". Museum.state.il.us. 2007-08-30. Retrieved 2012-02-12.
  31. ↑ Wang et al. (2005). "Modeling the Sun's Magnetic Field and Irradiance since 1713". The Astrophysical Journal 625 (1): 522–538. Bibcode:2005ApJ...625..522W. doi:10.1086/429689.
  32. ↑ Steinhilber et al. (2009). "Total solar irradiance since 1996: is there a long-term variation unrelated to solar surface magnetic phenomena?". Geophysical Research Letters 36: L19704. Bibcode:2010A&A...523A..39S. doi:10.1051/0004-6361/200811446.
  33. ↑ Vieira et al. (2011). "Evolution of the solar irradiance during the Holocene". Astronomy & Astrophysics 531: A6. Bibcode:2011A&A...531A...6V. doi:10.1051/0004-6361/201015843.
  34. ↑ Steinhilber et al. (2012). "9,400 years of cosmic radiation and solar activity from ice cores and tree rings". Proceedings of the National Academy of Sciences. doi:10.1073/pnas.1118965109.
  35. ↑ Osborne JE; Hutchinson PE (August 2002). "Vitamin D and systemic cancer: is this relevant to malignant melanoma?". Br. J. Dermatol. 147 (2): 197–213. doi:10.1046/j.1365-2133.2002.04960.x. PMID 12174089.
  36. ↑ "Dietary Supplement Fact Sheet: Vitamin D". Office of Dietary Supplements, National Institutes of Health.
  37. ↑ Cranney A; Horsley T; O'Donnell S; Weiler H et al. (August 2007). "Effectiveness and safety of vitamin D in relation to bone health". Evidence report/technology assessment (158): 1–235. PMID 18088161.
  38. ↑ John E; Schwartz G; Koo J; Van Den Berg D et al. (June 15, 2005). "Sun Exposure, Vitamin D Receptor Gene Polymorphisms, and Risk of Advanced Prostate Cancer". Cancer Research 65 (12): 5470–5479. doi:10.1158/0008-5472.can-04-3134.
  39. ↑ Egan K; Sosman J; Blot W (February 2, 2005). "Sunlight and Reduced Risk of Cancer: Is The Real Story Vitamin D?". J Natl Cancer Inst 97 (3): 161–163. doi:10.1093/jnci/dji047.
  40. ↑ Mead MN (April 2008). "Benefits of sunlight: a bright spot for human health". Environmental Health Perspectives 116 (4): A160–A167. doi:10.1289/ehp.116-a160. PMC 2290997. PMID 18414615.
  41. ↑ Lucas RM; Repacholi MH; McMichael AJ (June 2006). "Is the current public health message on UV exposure correct?". Bulletin of the World Health Organization 84 (6): 485–491. doi:10.2471/BLT.05.026559. PMC 2627377. PMID 16799733.
  42. ↑ "13th Report on Carcinogens: Ultraviolet-Radiation-Related Exposures" (PDF). National Toxicology Program. October 2014. Retrieved 2014-12-22.
  43. ↑ "Risks and Benefits" (PDF). Retrieved 2010-05-13.

Further reading

External links

Media related to Sunlight at Wikimedia Commons