Insight “Visible light” redirects here. For light that cannot be seen with human eye, see Electromagnetic radiation. For other uses,

see Light (disambiguation) and Visible light (disambiguation).

The Sun is Earth’s primary source of light. About 44% of the sun’s electromagnetic radiation that reaches the ground is in the visible light range.Visible light (commonly referred to simply as light) is electromagnetic radiation that is visible to the hu-man eye, and is responsible for the sense of sight.[1] Visible light has a wavelength in the range of about 380 nanometres (nm) to about 740 nanometres – be-tween the invisible infrared, with longer wavelengths and the invisible ultraviolet, with shorter wavelengths.Primary properties of visible light are intensity, prop-agation direction, frequency or wavelength spec-trum, and polarisation, while its speed in a vacuum, 299,792,458 meters per second, is one of the funda-mental constants of nature. Visible light, as with all types of electromagnetic radiation (EMR), is experimen-tally found to always move at this speed in vacuum.In common with all types of EMR, visible light is emit-ted and absorbed in tiny “packets” called photons, and exhibits properties of both waves and parti-cles. This property is referred to as the wave–par-ticle duality. The study of light, known as optics, is an important research area in modern physics.In physics, the term light sometimes refers to electro-magnetic radiation of any wavelength, whether visi-ble or not.This article focuses on visible light. See the electromagnetic radiation article for the general term.There are many sources of light. The most common light sources are thermal: a body at a given temperature emits

a characteristic spectrum of black-body radiation. A simple thermal source is sunlight, the radiation emit-ted by the chromosphere of the Sun at around 6,000 Kelvin peaks in the visible region of the electro-magnetic spectrum when plotted in wavelength units and roughly 44% of sunlight energy that reaches the ground is visible.Another example is incandescent light bulbs, which emit only around 10% of their energy as visible light and the remainder as infrared. A common thermal light source in history is the glowing solid particles in flames, but these also emit most of their radiation in the infrared, and only a fraction in the visible spectrum. The peak of the blackbody spectrum is in the deep infra-red, at about 10 micrometer wavelength, for relatively cool objects like human beings. As the temperature increases, the peak shifts to shorter wavelengths, producing first a red glow, then a white one, and finally a blue-white colour as the peak moves out of the visible part of the spectrum and into the ultraviolet. These colours can be seen when metal is heated to “red hot” or “white hot”. Blue-white thermal emission is not often seen, except in stars (the commonly seen pure-blue colour in a gas flame or a welder’s torch is in fact due to molecular emission, notably by CH radicals (emitting a wavelength band around 425 nm, and is not seen in stars or pure thermal radiation)).

a characteristic spectrum of black-body radiation. A simple thermal source is sunlight, the radiation emit-ted by the chromosphere of the Sun at around 6,000 Kelvin peaks in the visible region of the electro-magnetic spectrum when plotted in wavelength units and roughly 44% of sunlight energy that reaches the ground is visible.Another example is incandescent light bulbs, which emit only around 10% of their energy as visible light and the remainder as infrared. A common thermal light source in history is the glowing solid particles in flames, but these also emit most of their radiation in the infrared, and only a fraction in the visible spectrum. The peak of the blackbody spectrum is in the deep infra-red, at about 10 micrometer wavelength, for relatively cool objects like human beings. As the temperature increases, the peak shifts to shorter wavelengths, producing first a red glow, then a white one, and finally a blue-white colour as the peak moves out of the visible part of the spectrum and into the ultraviolet. These colours can be seen when metal is heated to “red hot” or “white hot”. Blue-white thermal emission is not often seen, except in stars (the commonly seen pure-blue colour in a gas flame or a welder’s torch is in fact due to molecular emission, notably by CH radicals (emitting a wavelength band around 425 nm, and is not seen in stars or pure thermal radiation)).

“There is a single light of science, and to brighten it anywhere is to brighten it

everywhere.”

- Isaac Asimov

“There is a single light of science, and to brighten it anywhere is to brighten it

everywhere.”

- Isaac Asimov

Spee

d of

Lig

ht

The s p e e d of light in a vacuum is defined to be exactly 299,792,458 m/s (approximately 186,282 miles per second). The fixed value of the speed of light in SI units results from the fact that the metre is now defined in terms of the speed of light. All forms of electromagnetic radiation are be-lieved to move at exactly this same speed in vacuum.Different physicists have attempted to measure the speed of light throughout history. Galileo attempted to measure the speed of light in the seventeenth cen-tury. An early experiment to measure the speed of light was conducted by Ole Rømer, a Danish phys-icist, in 1676. Using a telescope, Rømer observed the motions of Jupiter and one of its moons, Io. Not-ing discrepancies in the apparent period of Io’s or-bit, he calculated that light takes about 22 minutes to traverse the diameter of Earth’s orbit.[4] How-ever, its size was not known at that time. If Rømer had known the diameter of the Earth’s orbit, he would have calculated a speed of 227,000,000 m/s.Another, more accurate, measurement of the speed of light was performed in Europe by Hippolyte Fizeau in 1849. Fizeau directed a beam of light at a mirror several kilometers away. A rotating cog wheel was placed in the path of the light beam as it traveled from the source, to the mirror and then returned to its origin.

Fizeau found that at a certain rate of rotation, the beam would pass through one gap in the wheel on the way out and the next gap on the way back. Knowing the distance to the mirror, the number of teeth on the wheel, and the rate of rotation, Fizeau was able to calculate the speed of light as 313,000,000 m/s.Léon Foucault used an experiment which used ro-tating mirrors to obtain a value of 298,000,000 m/s in 1862. Albert A. Michelson conducted experiments on the speed of light from 1877 until his death in 1931. He refined Foucault’s methods in 1926 us-ing improved rotating mirrors to measure the time it took light to make a round trip from Mt. Wilson to Mt. San Antonio in California. The precise meas-urements yielded a speed of 299,796,000 m/s.The effective velocity of light in various transparent substances containing ordinary matter, is less than in

Fizeau found that at a certain rate of rotation, the beam would pass through one gap in the wheel on the way out and the next gap on the way back. Knowing the distance to the mirror, the number of teeth on the wheel, and the rate of rotation, Fizeau was able to calculate the speed of light as 313,000,000 m/s.Léon Foucault used an experiment which used ro-tating mirrors to obtain a value of 298,000,000 m/s in 1862. Albert A. Michelson conducted experiments on the speed of light from 1877 until his death in 1931. He refined Foucault’s methods in 1926 us-ing improved rotating mirrors to measure the time it took light to make a round trip from Mt. Wilson to Mt. San Antonio in California. The precise meas-urements yielded a speed of 299,796,000 m/s.The effective velocity of light in various transparent substances containing ordinary matter, is less than in

vac-u u m . For exam-ple the speed of light in water is about 3/4 of that in vacuum. Howev-er, the slowing process in matter is thought to result not from actual slowing of particles of light, but rather from their absorption and re-emission from charged particles in matter.As an extreme example of the nature of light-slowing in matter,

There are many sources of light. The most common light sources are thermal: a body at a given temperature emits a character-istic spectrum of black-body radiation. A simple thermal source is sunlight, the radi-ation emitted by the chromosphere of the Sun at around 6,000 Kelvin peaks in the visible region of the electromagnetic spec-trum when plotted in wavelength units and roughly 44% of sunlight energy that reach-es the ground is visible.[8] Another example is incandescent light bulbs, which emit only around 10% of their energy as visible light and the remainder as infrared. A common thermal light source in history is the glow-ing solid particles in flames, but these also emit most of their radiation in the infrared, and only a fraction in the visible spectrum. The peak of the blackbody spectrum is in the deep infrared, at about 10 micrometer wavelength, for relatively cool objects like human beings. As the temperature increas-es, the peak shifts to shorter wavelengths, producing first a red glow, then a white one, and finally a blue-white colour as the peak moves out of the visible part of the spectrum and into the ultraviolet. These colours can be seen when metal is heated to “red hot” or “white hot”. Blue-white thermal emission is not often seen, except in stars (the com-monly seen pure-blue colour in a gas flame or a welder’s torch is in fact due to molecular emission, notably by CH radicals (emitting a wavelength band around 425 nm, and is not seen in stars or pure thermal radiation)).Atoms emit and absorb light at characteris-tic energies. This produces “emission lines”

in the spectrum of each atom. Emission can be spontaneous, as in light-emitting diodes, gas discharge lamps (such as neon lamps and neon signs, mercury-vapor lamps, etc.), and flames (light from the hot gas itself—so, for example, sodium in a gas flame emits characteristic yellow light). Emission can also be stimulated, as in a laser or a microwave maser.Deceleration of a free charged particle, such as an electron, can produce visible radiation: cyclotron radiation, synchrotron radiation, and bremsstrahlung radiation are all examples of this. Particles moving through a medium faster than the speed of light in that medium can produce visible Cherenkov radiation.Certain chemicals produce visible radiation by chemoluminescence. In living things, this process is called bioluminescence. For example, fireflies produce light by this means, and boats moving through water can disturb plankton which produce a glow-ing wake.Certain substances produce light when they are illuminated by more energetic radiation, a process known as fluorescence. Some substances emit light slowly after excitation by more energetic radiation. This is known as phosphorescence.Phosphorescent materials can also be excited by bombarding them with subatom-ic particles. Cathodoluminescence is one example. This mechanism is used in cath-ode ray tube television sets and computer monitors.

Sources of LightM

an Made

There are many sources of light. The most com-mon light sources are thermal: a body at a given temperature emits a characteristic spectrum of black-body radiation. A simple thermal source is sunlight, the radiation emitted by the chromosphere of the Sun at around 6,000 Kelvin peaks in the vis-ible region of the electromagnetic spectrum when plotted in wavelength units and roughly 44% of sunlight energy that reaches the ground is visible.[8] Another example is incandescent light bulbs, which emit only around 10% of their energy as vis-ible light and the remainder as infrared. A common thermal light source in history is the glowing sol-id particles in flames, but these also emit most of their radiation in the infrared, and only a fraction in the visible spectrum. The peak of the blackbody spectrum is in the deep infrared, at about 10 mi-crometer wavelength, for relatively cool objects like human beings. As the temperature increases, the peak shifts to shorter wavelengths, producing first a red glow, then a white one, and finally a blue-white colour as the peak moves out of the visible part of the spectrum and into the ultraviolet. These colours can be seen when metal is heated to “red hot” or “white hot”. Blue-white thermal emission is not of-ten seen, except in stars (the commonly seen pure-blue colour in a gas flame or a welder’s torch is in fact due to molecular emission, notably by CH rad-icals (emitting a wavelength band around 425 nm, and is not seen in stars or pure thermal radiation)).

Sources of Light

There are many sources of light. The most com-mon light sources are thermal: a body at a given temperature emits a characteristic spectrum of black-body radiation. A simple thermal source is sunlight, the radiation emitted by the chromosphere of the Sun at around 6,000 Kelvin peaks in the vis-ible region of the electromagnetic spectrum when plotted in wavelength units and roughly 44% of sunlight energy that reaches the ground is visible.[8] Another example is incandescent light bulbs, which emit only around 10% of their energy as vis-ible light and the remainder as infrared. A common thermal light source in history is the glowing sol-id particles in flames, but these also emit most of their radiation in the infrared, and only a fraction in the visible spectrum. The peak of the blackbody spectrum is in the deep infrared, at about 10 mi-crometer wavelength, for relatively cool objects like human beings. As the temperature increases, the peak shifts to shorter wavelengths, producing first a red glow, then a white one, and finally a blue-white colour as the peak moves out of the visible part of the spectrum and into the ultraviolet. These colours can be seen when metal is heated to “red hot” or “white hot”. Blue-white thermal emission is not of-ten seen, except in stars (the commonly seen pure-blue colour in a gas flame or a welder’s torch is in fact due to molecular emission, notably by CH rad-icals (emitting a wavelength band around 425 nm, and is not seen in stars or pure thermal radiation)).

Atoms emit and absorb light at characteristic en-ergies. This produces “emission lines” in the spec-trum of each atom. Emission can be spontaneous, as in light-emitting diodes, gas discharge lamps (such as neon lamps and neon signs, mercury-va-por lamps, etc.), and flames (light from the hot gas itself—so, for example, sodium in a gas flame emits characteristic yellow light). Emission can also be stimulated, as in a laser or a microwave maser.Deceleration of a free charged particle, such as an electron, can produce visible radiation: cyclotron ra-diation, synchrotron radiation, and bremsstrahlung radiation are all examples of this. Particles moving through a medium faster than the speed of light in that medium can produce visible Cherenkov radiation.Certain chemicals produce visible radiation by chemo-luminescence. In living things, this process is called bioluminescence. For example, fireflies produce light by this means, and boats moving through water can disturb plankton which produce a glowing wake.Certain substances produce light when they are illuminated by more energetic radiation, a pro-cess known as fluorescence. Some substances emit light slowly after excitation by more energet-ic radiation. This is known as phosphorescence.Phosphorescent materials can also be excit-ed by bombarding them with subatomic par-ticles. Cathodoluminescence is one exam-ple. This mechanism is used in cathode ray tube television sets and computer monitors.

Sources of LightN

atural

Light in NaturePhotosynthesis is a 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. Carbohydrates, such as sugars, are synthesized from carbon dioxide and water (hence the name photosynthesis, from the Greek φώτο- [photo-], “light,” and σύνθεσις [synthesis], “putting together”) during the process. Oxygen is also released, mostly as a waste product. Most plants, most algae, and cyanobacteria perform the process of photosynthesis, and are called photoautotrophs. Photosynthesis maintains atmospheric oxygen levels and supplies most of the energy necessary for all life on Earth,[1] except for chemotrophs, which gain energy through oxidative

chemical reactions. Although photosynthesis is performed differently by different species, the process always begins when energy from light is absorbed by proteins called reaction centres that contain green chlorophyll pigments. In plants, these proteins are held inside organelles called chloroplasts, which are most abundant in leaf cells, while in bacteria they are embedded in the plasma membrane. In these light-dependent reactions, some energy is used to strip electrons from suitable substances such as water. This produces oxygen gas and hydrogen ions, which are transferred to a compound called nicotinamide adenine dinucleotide phosphate (NADP+), reducing it to NADPH. More light energy is transferred to chemical energy in the generation of adenosine

triphosphate (ATP), the “energy currency” of cells. In plants, algae and cyanobacteria, sugars are produced by a sequence of light-independent reactions called the Calvin cycle, but some bacteria use different mechanisms, such as the reverse Krebs cycle. In the Calvin cycle, atmospheric carbon dioxide is incorporated into already existing organic carbon compounds, such as ribulose bisphosphate (RuBP).[2] Using the ATP and NADPH produced by the light-dependent reactions, the resulting compounds are then reduced into triose phosphate. Of every six triose phosphate molecules produced, one is removed to form further carbohydrates and five are “recycled” back into the cycle to regenerate the original carbon dioxide acceptor, RuBP.Ph

otos

ynth

esis

triphosphate (ATP), the “energy currency” of cells. In plants, algae and cyanobacteria, sugars are produced by a sequence of light-independent reactions called the Calvin cycle, but some bacteria use different mechanisms, such as the reverse Krebs cycle. In the Calvin cycle, atmospheric carbon dioxide is incorporated into already existing organic carbon compounds, such as ribulose bisphosphate (RuBP).[2] Using the ATP and NADPH produced by the light-dependent reactions, the resulting compounds are then reduced into triose phosphate. Of every six triose phosphate molecules produced, one is removed to form further carbohydrates and five are “recycled” back into the cycle to regenerate the original carbon dioxide acceptor, RuBP.

“Science never solves a problem without creating

ten more”

- George Bernard Shaw

“Science never solves a problem without creating

ten more”

- George Bernard Shaw