Photons are emitted in a threaded laser beam | |

Composition | Elementary particle |
---|---|

Statistics | Bose–Einstein |

Interactions | Electromagnetic, Weak, Gravity |

Symbol | γ |

Theorized | Albert Einstein (1905) The name of "photon" is generally attributed to Gilbert N. Lewis (1926) |

Mass | 0 <1×10 ^{−18} eV/c^{2} ^{ [1] } |

Mean lifetime | Stable^{ [1] } |

Electric charge | 0 <1×10 ^{−35} e ^{ [1] } |

Spin | 1 |

Parity | −1^{ [1] } |

C parity | −1^{ [1] } |

Condensed | I ( J ^{ P C })=0,1(1^{−−})^{ [1] } |

The **photon** is a type of elementary particle. It is the quantum of the electromagnetic field including electromagnetic radiation such as light and radio waves, and the force carrier for the electromagnetic force. Photons are massless,^{ [lower-alpha 1] } and they always move at the speed of light in vacuum, 299792458 m/s.

- Nomenclature
- Physical properties
- Relativistic energy and momentum
- Experimental checks on photon mass
- Historical development
- Wave–particle duality and uncertainty principles
- Bose–Einstein model of a photon gas
- Stimulated and spontaneous emission
- Quantum field theory
- Quantization of the electromagnetic field
- As a gauge boson
- Hadronic properties
- Contributions to the mass of a system
- In matter
- Technological applications
- Quantum optics and computation
- See also
- Notes
- References
- Further reading
- External links

Like all elementary particles, photons are currently best explained by quantum mechanics and exhibit wave–particle duality, their behavior featuring properties of both waves and particles.^{ [2] } The modern photon concept originated during the first two decades of the 20th century with the work of Albert Einstein, who built upon the research of Max Planck. While trying to explain how matter and electromagnetic radiation could be in thermal equilibrium with one another, Planck proposed that the energy stored within a material object should be regarded as composed of an integer number of discrete, equal-sized parts. Einstein introduced the idea that light itself is made of discrete units of energy. Experiments validated Einstein's approach,^{ [3] }^{ [4] }^{ [5] } and in 1926, Gilbert N. Lewis popularized the term *photon* for these energy units.^{ [6] }^{ [7] }^{ [8] }

In the Standard Model of particle physics, photons and other elementary particles are described as a necessary consequence of physical laws having a certain symmetry at every point in spacetime. The intrinsic properties of particles, such as charge, mass, and spin, are determined by this gauge symmetry. The photon concept has led to momentous advances in experimental and theoretical physics, including lasers, Bose–Einstein condensation, quantum field theory, and the probabilistic interpretation of quantum mechanics. It has been applied to photochemistry, high-resolution microscopy, and measurements of molecular distances. Recently, photons have been studied as elements of quantum computers, and for applications in optical imaging and optical communication such as quantum cryptography.

The word *quanta* (singular *quantum,* Latin for * how much *) was used before 1900 to mean particles or amounts of different quantities, including electricity. In 1900, the German physicist Max Planck was studying black-body radiation, and he suggested that the experimental observations, specifically at shorter wavelengths, would be explained if the energy stored within a molecule was a "discrete quantity composed of an integral number of finite equal parts", which he called "energy elements".^{ [9] } In 1905, Albert Einstein published a paper in which he proposed that many light-related phenomena—including black-body radiation and the photoelectric effect—would be better explained by modelling electromagnetic waves as consisting of spatially localized, discrete wave-packets.^{ [10] } He called such a wave-packet *the light quantum* (German: *das Lichtquant*).^{ [lower-alpha 2] }

The name *photon* derives from the Greek word for light, *φῶς* (transliterated *phôs*). Arthur Compton used *photon* in 1928, referring to Gilbert N. Lewis, who coined the term in a letter to * Nature * on December 18, 1926.^{ [6] }^{ [11] } The same name was used earlier but was never widely adopted before Lewis: in 1916 by the American physicist and psychologist Leonard T. Troland, in 1921 by the Irish physicist John Joly, in 1924 by the French physiologist René Wurmser (1890–1993), and in 1926 by the French physicist Frithiof Wolfers (1891–1971).^{ [8] } The name was suggested initially as a unit related to the illumination of the eye and the resulting sensation of light and was used later in a physiological context. Although Wolfers's and Lewis's theories were contradicted by many experiments and never accepted, the new name was adopted very soon by most physicists after Compton used it.^{ [8] }^{ [lower-alpha 3] }

In physics, a photon is usually denoted by the symbol *γ* (the Greek letter gamma). This symbol for the photon probably derives from gamma rays, which were discovered in 1900 by Paul Villard,^{ [13] }^{ [14] } named by Ernest Rutherford in 1903, and shown to be a form of electromagnetic radiation in 1914 by Rutherford and Edward Andrade.^{ [15] } In chemistry and optical engineering, photons are usually symbolized by *hν*, which is the photon energy, where *h* is Planck constant and the Greek letter *ν* (nu) is the photon's frequency.^{ [16] } Much less commonly, the photon can be symbolized by *hf*, where its frequency is denoted by *f*.^{ [17] }

A photon is massless,^{ [lower-alpha 4] } has no electric charge,^{ [18] }^{ [19] } and is a stable particle. In vacuum, a photon has two possible polarization states.^{ [20] } The photon is the gauge boson for electromagnetism,^{ [21] }^{:29–30} and therefore all other quantum numbers of the photon (such as lepton number, baryon number, and flavour quantum numbers) are zero.^{ [22] } Also, the photon does not obey the Pauli exclusion principle, but instead obeys Bose–Einstein statistics.^{ [23] }^{:1221}

Photons are emitted in many natural processes. For example, when a charge is accelerated it emits synchrotron radiation. During a molecular, atomic or nuclear transition to a lower energy level, photons of various energy will be emitted, ranging from radio waves to gamma rays. Photons can also be emitted when a particle and its corresponding antiparticle are annihilated (for example, electron–positron annihilation).^{ [23] }^{:572,1114,1172}

In empty space, the photon moves at *c* (the speed of light) and its energy and momentum are related by *E* = *pc*, where *p* is the magnitude of the momentum vector * p*. This derives from the following relativistic relation, with

The energy and momentum of a photon depend only on its frequency (*) or inversely, its wavelength (**λ*):

where * k* is the wave vector (where the wave number

Since * p* points in the direction of the photon's propagation, the magnitude of the momentum is

The photon also carries a quantity called spin angular momentum that does not depend on its frequency.^{ [26] } Because photons always move at the speed of light, the spin is best expressed in terms of the component measured along its direction of motion, its helicity, which must be ±*ħ*. These two possible helicities, called right-handed and left-handed, correspond to the two possible circular polarization states of the photon.^{ [27] }

To illustrate the significance of these formulae, the annihilation of a particle with its antiparticle in free space must result in the creation of at least *two* photons for the following reason. In the center of momentum frame, the colliding antiparticles have no net momentum, whereas a single photon always has momentum (since, as we have seen, it is determined by the photon's frequency or wavelength, which cannot be zero). Hence, conservation of momentum (or equivalently, translational invariance) requires that at least two photons are created, with zero net momentum. (However, it is possible if the system interacts with another particle or field for the annihilation to produce one photon, as when a positron annihilates with a bound atomic electron, it is possible for only one photon to be emitted, as the nuclear Coulomb field breaks translational symmetry.)^{ [28] }^{:64–65} The energy of the two photons, or, equivalently, their frequency, may be determined from conservation of four-momentum.

Seen another way, the photon can be considered as its own antiparticle (thus an "antiphoton" is simply a normal photon). The reverse process, pair production, is the dominant mechanism by which high-energy photons such as gamma rays lose energy while passing through matter.^{ [29] } That process is the reverse of "annihilation to one photon" allowed in the electric field of an atomic nucleus.

The classical formulae for the energy and momentum of electromagnetic radiation can be re-expressed in terms of photon events. For example, the pressure of electromagnetic radiation on an object derives from the transfer of photon momentum per unit time and unit area to that object, since pressure is force per unit area and force is the change in momentum per unit time.^{ [30] }

Each photon carries two distinct and independent forms of angular momentum of light. The spin angular momentum of light of a particular photon is always either +*ħ* or −*ħ*. The light orbital angular momentum of a particular photon can be any integer *N*, including zero.^{ [31] }

Current commonly accepted physical theories imply or assume the photon to be strictly massless. If the photon is not a strictly massless particle, it would not move at the exact speed of light, *c*, in vacuum. Its speed would be lower and depend on its frequency. Relativity would be unaffected by this; the so-called speed of light, *c*, would then not be the actual speed at which light moves, but a constant of nature which is the upper bound on speed that any object could theoretically attain in spacetime.^{ [32] } Thus, it would still be the speed of spacetime ripples (gravitational waves and gravitons), but it would not be the speed of photons.

If a photon did have non-zero mass, there would be other effects as well. Coulomb's law would be modified and the electromagnetic field would have an extra physical degree of freedom. These effects yield more sensitive experimental probes of the photon mass than the frequency dependence of the speed of light. If Coulomb's law is not exactly valid, then that would allow the presence of an electric field to exist within a hollow conductor when it is subjected to an external electric field. This provides a means for very-high-precision tests of Coulomb's law.^{ [33] } A null result of such an experiment has set a limit of *m* ≲ 10^{−14} eV/*c*^{2}.^{ [34] }

Sharper upper limits on the speed of light have been obtained in experiments designed to detect effects caused by the galactic vector potential. Although the galactic vector potential is very large because the galactic magnetic field exists on very great length scales, only the magnetic field would be observable if the photon is massless. In the case that the photon has mass, the mass term 1/2*m*^{2}*A*_{μ}*A*^{μ} would affect the galactic plasma. The fact that no such effects are seen implies an upper bound on the photon mass of *m*<3×10^{−27} eV/*c*^{2}.^{ [35] } The galactic vector potential can also be probed directly by measuring the torque exerted on a magnetized ring.^{ [36] } Such methods were used to obtain the sharper upper limit of 1.07×10^{−27} eV/*c*^{2} (the equivalent of 10^{−36} daltons ) given by the Particle Data Group.^{ [37] }

These sharp limits from the non-observation of the effects caused by the galactic vector potential have been shown to be model-dependent.^{ [38] } If the photon mass is generated via the Higgs mechanism then the upper limit of *m* ≲ 10^{−14} eV/*c*^{2} from the test of Coulomb's law is valid.

In most theories up to the eighteenth century, light was pictured as being made up of particles. Since particle models cannot easily account for the refraction, diffraction and birefringence of light, wave theories of light were proposed by René Descartes (1637),^{ [39] } Robert Hooke (1665),^{ [40] } and Christiaan Huygens (1678);^{ [41] } however, particle models remained dominant, chiefly due to the influence of Isaac Newton.^{ [42] } In the early nineteenth century, Thomas Young and August Fresnel clearly demonstrated the interference and diffraction of light and by 1850 wave models were generally accepted.^{ [43] } In 1865, James Clerk Maxwell's prediction ^{ [44] } that light was an electromagnetic wave—which was confirmed experimentally in 1888 by Heinrich Hertz's detection of radio waves ^{ [45] }—seemed to be the final blow to particle models of light.

The Maxwell wave theory, however, does not account for *all* properties of light. The Maxwell theory predicts that the energy of a light wave depends only on its intensity, not on its frequency; nevertheless, several independent types of experiments show that the energy imparted by light to atoms depends only on the light's frequency, not on its intensity. For example, some chemical reactions are provoked only by light of frequency higher than a certain threshold; light of frequency lower than the threshold, no matter how intense, does not initiate the reaction. Similarly, electrons can be ejected from a metal plate by shining light of sufficiently high frequency on it (the photoelectric effect); the energy of the ejected electron is related only to the light's frequency, not to its intensity.^{ [46] }^{ [lower-alpha 5] }

At the same time, investigations of black-body radiation carried out over four decades (1860–1900) by various researchers^{ [47] } culminated in Max Planck's hypothesis ^{ [48] }^{ [49] } that the energy of *any* system that absorbs or emits electromagnetic radiation of frequency *ν* is an integer multiple of an energy quantum *E* = *hν*. As shown by Albert Einstein,^{ [10] }^{ [50] } some form of energy quantization *must* be assumed to account for the thermal equilibrium observed between matter and electromagnetic radiation; for this explanation of the photoelectric effect, Einstein received the 1921 Nobel Prize in physics.^{ [51] }

Since the Maxwell theory of light allows for all possible energies of electromagnetic radiation, most physicists assumed initially that the energy quantization resulted from some unknown constraint on the matter that absorbs or emits the radiation. In 1905, Einstein was the first to propose that energy quantization was a property of electromagnetic radiation itself.^{ [10] } Although he accepted the validity of Maxwell's theory, Einstein pointed out that many anomalous experiments could be explained if the *energy* of a Maxwellian light wave were localized into point-like quanta that move independently of one another, even if the wave itself is spread continuously over space.^{ [10] } In 1909^{ [50] } and 1916,^{ [52] } Einstein showed that, if Planck's law of black-body radiation is accepted, the energy quanta must also carry momentum *p* = *h*/*λ*, making them full-fledged particles. This photon momentum was observed experimentally^{ [53] } by Arthur Compton, for which he received the Nobel Prize in 1927. The pivotal question was then: how to unify Maxwell's wave theory of light with its experimentally observed particle nature? The answer to this question occupied Albert Einstein for the rest of his life,^{ [54] } and was solved in quantum electrodynamics and its successor, the Standard Model (see * § Second quantization * and * § The photon as a gauge boson *, below).

Einstein's 1905 predictions were verified experimentally in several ways in the first two decades of the 20th century, as recounted in Robert Millikan's Nobel lecture.^{ [55] } However, before Compton's experiment ^{ [53] } showed that photons carried momentum proportional to their wave number (1922), most physicists were reluctant to believe that electromagnetic radiation itself might be particulate. (See, for example, the Nobel lectures of Wien,^{ [47] } Planck ^{ [49] } and Millikan.^{ [55] }) Instead, there was a widespread belief that energy quantization resulted from some unknown constraint on the matter that absorbed or emitted radiation. Attitudes changed over time. In part, the change can be traced to experiments such as Compton scattering, where it was much more difficult not to ascribe quantization to light itself to explain the observed results.^{ [56] }

Even after Compton's experiment, Niels Bohr, Hendrik Kramers and John Slater made one last attempt to preserve the Maxwellian continuous electromagnetic field model of light, the so-called BKS theory.^{ [57] } An important feature of the BKS theory is how it treated the conservation of energy and the conservation of momentum. In the BKS theory, energy and momentum are only conserved on the average across many interactions between matter and radiation. However, refined Compton experiments showed that the conservation laws hold for individual interactions.^{ [58] } Accordingly, Bohr and his co-workers gave their model "as honorable a funeral as possible".^{ [54] } Nevertheless, the failures of the BKS model inspired Werner Heisenberg in his development of matrix mechanics.^{ [59] }

A few physicists persisted^{ [60] } in developing semiclassical models in which electromagnetic radiation is not quantized, but matter appears to obey the laws of quantum mechanics. Although the evidence from chemical and physical experiments for the existence of photons was overwhelming by the 1970s, this evidence could not be considered as *absolutely* definitive; since it relied on the interaction of light with matter, and a sufficiently complete theory of matter could in principle account for the evidence. Nevertheless, *all* semiclassical theories were refuted definitively in the 1970s and 1980s by photon-correlation experiments.^{ [lower-alpha 6] } Hence, Einstein's hypothesis that quantization is a property of light itself is considered to be proven.

Photons obey the laws of quantum mechanics, and so their behavior has both wave-like and particle-like aspects. When a photon is detected by a measuring instrument, it is registered as a single, particulate unit. However, the *probability* of detecting a photon is calculated by equations that describe waves. This combination of aspects is known as wave–particle duality. For example, the probability distribution for the location at which a photon might be detected displays clearly wave-like phenomena such as diffraction and interference. A single photon passing through a double-slit experiment lands on the screen with a probability distribution given by its interference pattern determined by Maxwell's equations.^{ [61] } However, experiments confirm that the photon is *not* a short pulse of electromagnetic radiation; it does not spread out as it propagates, nor does it divide when it encounters a beam splitter.^{ [62] } Rather, the photon seems to be a point-like particle since it is absorbed or emitted *as a whole* by arbitrarily small systems, including systems much smaller than its wavelength, such as an atomic nucleus (≈10^{−15} m across) or even the point-like electron.

While many introductory texts treat photons using the mathematical techniques of non-relativistic quantum mechanics, this is in some ways an awkward oversimplification, as photons are by nature intrinsically relativistic. Because photons have zero rest mass, no wave function defined for a photon can have all the properties familiar from wave functions in non-relativistic quantum mechanics.^{ [lower-alpha 7] } In order to avoid these difficulties, physicists employ the second-quantized theory of photons described below, quantum electrodynamics, in which photons are quantized excitations of electromagnetic modes.^{ [67] }

Another difficulty is finding the proper analogue for the uncertainty principle, an idea frequently attributed to Heisenberg, who introduced the concept in analyzing a thought experiment involving an electron and a high-energy photon. However, Heisenberg did not give precise mathematical definitions of what the "uncertainty" in these measurements meant. The precise mathematical statement of the position–momentum uncertainty principle is due to Kennard, Pauli, and Weyl.^{ [68] }^{ [69] } The uncertainty principle applies to situations where an experimenter has a choice of measuring either one of two "canonically conjugate" quantities, like the position and the momentum of a particle. According to the uncertainty principle, no matter how the particle is prepared, it is not possible to make a precise prediction for both of the two alternative measurements: if the outcome of the position measurement is made more certain, the outcome of the momentum measurement becomes less so, and vice versa.^{ [70] } A coherent state minimizes the overall uncertainty as far as quantum mechanics allows.^{ [67] } Quantum optics makes use of coherent states for modes of the electromagnetic field. There is a tradeoff, reminiscent of the position–momentum uncertainty relation, between measurements of an electromagnetic wave's amplitude and its phase.^{ [67] } This is sometimes informally expressed in terms of the uncertainty in the number of photons present in the electromagnetic wave, , and the uncertainty in the phase of the wave, . However, this cannot be an uncertainty relation of the Kennard–Pauli–Weyl type, since unlike position and momentum, the phase cannot be represented by a Hermitian operator.^{ [71] }

In 1924, Satyendra Nath Bose derived Planck's law of black-body radiation without using any electromagnetism, but rather by using a modification of coarse-grained counting of phase space.^{ [72] } Einstein showed that this modification is equivalent to assuming that photons are rigorously identical and that it implied a "mysterious non-local interaction",^{ [73] }^{ [74] } now understood as the requirement for a symmetric quantum mechanical state. This work led to the concept of coherent states and the development of the laser. In the same papers, Einstein extended Bose's formalism to material particles (bosons) and predicted that they would condense into their lowest quantum state at low enough temperatures; this Bose–Einstein condensation was observed experimentally in 1995.^{ [75] } It was later used by Lene Hau to slow, and then completely stop, light in 1999^{ [76] } and 2001.^{ [77] }

The modern view on this is that photons are, by virtue of their integer spin, bosons (as opposed to fermions with half-integer spin). By the spin-statistics theorem, all bosons obey Bose–Einstein statistics (whereas all fermions obey Fermi–Dirac statistics).^{ [78] }

In 1916, Albert Einstein showed that Planck's radiation law could be derived from a semi-classical, statistical treatment of photons and atoms, which implies a link between the rates at which atoms emit and absorb photons. The condition follows from the assumption that functions of the emission and absorption of radiation by the atoms are independent of each other, and that thermal equilibrium is made by way of the radiation's interaction with the atoms. Consider a cavity in thermal equilibrium with all parts of itself and filled with electromagnetic radiation and that the atoms can emit and absorb that radiation. Thermal equilibrium requires that the energy density of photons with frequency (which is proportional to their number density) is, on average, constant in time; hence, the rate at which photons of any particular frequency are *emitted* must equal the rate at which they are *absorbed*.^{ [79] }

Einstein began by postulating simple proportionality relations for the different reaction rates involved. In his model, the rate for a system to *absorb* a photon of frequency and transition from a lower energy to a higher energy is proportional to the number of atoms with energy and to the energy density of ambient photons of that frequency,

where is the rate constant for absorption. For the reverse process, there are two possibilities: spontaneous emission of a photon, or the emission of a photon initiated by the interaction of the atom with a passing photon and the return of the atom to the lower-energy state. Following Einstein's approach, the corresponding rate for the emission of photons of frequency and transition from a higher energy to a lower energy is

where is the rate constant for emitting a photon spontaneously, and is the rate constant for emissions in response to ambient photons (induced or stimulated emission). In thermodynamic equilibrium, the number of atoms in state and those in state must, on average, be constant; hence, the rates and must be equal. Also, by arguments analogous to the derivation of Boltzmann statistics, the ratio of and is where and are the degeneracy of the state and that of , respectively, and their energies, the Boltzmann constant and the system's temperature. From this, it is readily derived that and

The and are collectively known as the *Einstein coefficients*.^{ [80] }

Einstein could not fully justify his rate equations, but claimed that it should be possible to calculate the coefficients , and once physicists had obtained "mechanics and electrodynamics modified to accommodate the quantum hypothesis".^{ [81] } Not long thereafter, in 1926, Paul Dirac derived the rate constants by using a semiclassical approach,^{ [82] } and, in 1927, succeeded in deriving *all* the rate constants from first principles within the framework of quantum theory.^{ [83] }^{ [84] } Dirac's work was the foundation of quantum electrodynamics, i.e., the quantization of the electromagnetic field itself. Dirac's approach is also called *second quantization* or quantum field theory;^{ [85] }^{ [86] }^{ [87] } earlier quantum mechanical treatments only treat material particles as quantum mechanical, not the electromagnetic field.

Einstein was troubled by the fact that his theory seemed incomplete, since it did not determine the *direction* of a spontaneously emitted photon. A probabilistic nature of light-particle motion was first considered by Newton in his treatment of birefringence and, more generally, of the splitting of light beams at interfaces into a transmitted beam and a reflected beam. Newton hypothesized that hidden variables in the light particle determined which of the two paths a single photon would take.^{ [42] } Similarly, Einstein hoped for a more complete theory that would leave nothing to chance, beginning his separation^{ [54] } from quantum mechanics. Ironically, Max Born's probabilistic interpretation of the wave function ^{ [88] }^{ [89] } was inspired by Einstein's later work searching for a more complete theory.^{ [90] }

In 1910, Peter Debye derived Planck's law of black-body radiation from a relatively simple assumption.^{ [91] } He decomposed the electromagnetic field in a cavity into its Fourier modes, and assumed that the energy in any mode was an integer multiple of , where is the frequency of the electromagnetic mode. Planck's law of black-body radiation follows immediately as a geometric sum. However, Debye's approach failed to give the correct formula for the energy fluctuations of black-body radiation, which were derived by Einstein in 1909.^{ [50] }

In 1925, Born, Heisenberg and Jordan reinterpreted Debye's concept in a key way.^{ [92] } As may be shown classically, the Fourier modes of the electromagnetic field—a complete set of electromagnetic plane waves indexed by their wave vector * k* and polarization state—are equivalent to a set of uncoupled simple harmonic oscillators. Treated quantum mechanically, the energy levels of such oscillators are known to be , where is the oscillator frequency. The key new step was to identify an electromagnetic mode with energy as a state with photons, each of energy . This approach gives the correct energy fluctuation formula.

Dirac took this one step further.^{ [83] }^{ [84] } He treated the interaction between a charge and an electromagnetic field as a small perturbation that induces transitions in the photon states, changing the numbers of photons in the modes, while conserving energy and momentum overall. Dirac was able to derive Einstein's and coefficients from first principles, and showed that the Bose–Einstein statistics of photons is a natural consequence of quantizing the electromagnetic field correctly (Bose's reasoning went in the opposite direction; he derived Planck's law of black-body radiation by *assuming* B–E statistics). In Dirac's time, it was not yet known that all bosons, including photons, must obey Bose–Einstein statistics.

Dirac's second-order perturbation theory can involve virtual photons, transient intermediate states of the electromagnetic field; the static electric and magnetic interactions are mediated by such virtual photons. In such quantum field theories, the probability amplitude of observable events is calculated by summing over *all* possible intermediate steps, even ones that are unphysical; hence, virtual photons are not constrained to satisfy , and may have extra polarization states; depending on the gauge used, virtual photons may have three or four polarization states, instead of the two states of real photons. Although these transient virtual photons can never be observed, they contribute measurably to the probabilities of observable events. Indeed, such second-order and higher-order perturbation calculations can give apparently infinite contributions to the sum. Such unphysical results are corrected for using the technique of renormalization.^{ [93] }

Other virtual particles may contribute to the summation as well; for example, two photons may interact indirectly through virtual electron–positron pairs.^{ [94] } Such photon–photon scattering (see two-photon physics), as well as electron–photon scattering, is meant to be one of the modes of operations of the planned particle accelerator, the International Linear Collider.^{ [95] }

In modern physics notation, the quantum state of the electromagnetic field is written as a Fock state, a tensor product of the states for each electromagnetic mode

where represents the state in which photons are in the mode . In this notation, the creation of a new photon in mode (e.g., emitted from an atomic transition) is written as . This notation merely expresses the concept of Born, Heisenberg and Jordan described above, and does not add any physics.

The electromagnetic field can be understood as a gauge field, i.e., as a field that results from requiring that a gauge symmetry holds independently at every position in spacetime.^{ [96] } For the electromagnetic field, this gauge symmetry is the Abelian U(1) symmetry of complex numbers of absolute value 1, which reflects the ability to vary the phase of a complex field without affecting observables or real valued functions made from it, such as the energy or the Lagrangian.

The quanta of an Abelian gauge field must be massless, uncharged bosons, as long as the symmetry is not broken; hence, the photon is predicted to be massless, and to have zero electric charge and integer spin. The particular form of the electromagnetic interaction specifies that the photon must have spin ±1; thus, its helicity must be . These two spin components correspond to the classical concepts of right-handed and left-handed circularly polarized light. However, the transient virtual photons of quantum electrodynamics may also adopt unphysical polarization states.^{ [96] }

In the prevailing Standard Model of physics, the photon is one of four gauge bosons in the electroweak interaction; the other three are denoted W^{+}, W^{−} and Z^{0} and are responsible for the weak interaction. Unlike the photon, these gauge bosons have mass, owing to a mechanism that breaks their SU(2) gauge symmetry. The unification of the photon with W and Z gauge bosons in the electroweak interaction was accomplished by Sheldon Glashow, Abdus Salam and Steven Weinberg, for which they were awarded the 1979 Nobel Prize in physics.^{ [97] }^{ [98] }^{ [99] } Physicists continue to hypothesize grand unified theories that connect these four gauge bosons with the eight gluon gauge bosons of quantum chromodynamics; however, key predictions of these theories, such as proton decay, have not been observed experimentally.^{ [100] }

Measurements of the interaction between energetic photons and hadrons show that the interaction is much more intense than expected by the interaction of merely photons with the hadron's electric charge. Furthermore, the interaction of energetic photons with protons is similar to the interaction of photons with neutrons^{ [101] } in spite of the fact that the electric charge structures of protons and neutrons are substantially different. A theory called Vector Meson Dominance (VMD) was developed to explain this effect. According to VMD, the photon is a superposition of the pure electromagnetic photon which interacts only with electric charges and vector mesons.^{ [102] } However, if experimentally probed at very short distances, the intrinsic structure of the photon is recognized as a flux of quark and gluon components, quasi-free according to asymptotic freedom in QCD and described by the photon structure function.^{ [103] }^{ [104] } A comprehensive comparison of data with theoretical predictions was presented in a review in 2000.^{ [105] }

The energy of a system that emits a photon is *decreased* by the energy of the photon as measured in the rest frame of the emitting system, which may result in a reduction in mass in the amount . Similarly, the mass of a system that absorbs a photon is *increased* by a corresponding amount. As an application, the energy balance of nuclear reactions involving photons is commonly written in terms of the masses of the nuclei involved, and terms of the form for the gamma photons (and for other relevant energies, such as the recoil energy of nuclei).^{ [106] }

This concept is applied in key predictions of quantum electrodynamics (QED, see above). In that theory, the mass of electrons (or, more generally, leptons) is modified by including the mass contributions of virtual photons, in a technique known as renormalization. Such "radiative corrections" contribute to a number of predictions of QED, such as the magnetic dipole moment of leptons, the Lamb shift, and the hyperfine structure of bound lepton pairs, such as muonium and positronium.^{ [107] }

Since photons contribute to the stress–energy tensor, they exert a gravitational attraction on other objects, according to the theory of general relativity. Conversely, photons are themselves affected by gravity; their normally straight trajectories may be bent by warped spacetime, as in gravitational lensing, and their frequencies may be lowered by moving to a higher gravitational potential, as in the Pound–Rebka experiment. However, these effects are not specific to photons; exactly the same effects would be predicted for classical electromagnetic waves.^{ [108] }

Light that travels through transparent matter does so at a lower speed than *c*, the speed of light in a vacuum. The factor by which the speed is decreased is called the refractive index of the material. In a classical wave picture, the slowing can be explained by the light inducing electric polarization in the matter, the polarized matter radiating new light, and that new light interfering with the original light wave to form a delayed wave. In a particle picture, the slowing can instead be described as a blending of the photon with quantum excitations of the matter to produce quasi-particles known as polariton (see this list for some other quasi-particles); this polariton has a nonzero effective mass, which means that it cannot travel at *c*. Light of different frequencies may travel through matter at different speeds; this is called dispersion (not to be confused with scattering). In some cases, it can result in extremely slow speeds of light in matter. The effects of photon interactions with other quasi-particles may be observed directly in Raman scattering and Brillouin scattering.^{ [109] }

Photons can be scattered by matter. For example, photons engage in so many collisions on the way from the core of the Sun that radiant energy can take about a million years to reach the surface;^{ [110] } however, once in open space, a photon takes only 8.3 minutes to reach Earth.^{ [111] }

Photons can also be absorbed by nuclei, atoms or molecules, provoking transitions between their energy levels. A classic example is the molecular transition of retinal (C_{20}H_{28}O), which is responsible for vision, as discovered in 1958 by Nobel laureate biochemist George Wald and co-workers. The absorption provokes a cis–trans isomerization that, in combination with other such transitions, is transduced into nerve impulses. The absorption of photons can even break chemical bonds, as in the photodissociation of chlorine; this is the subject of photochemistry.^{ [112] }^{ [113] }

Photons have many applications in technology. These examples are chosen to illustrate applications of photons *per se*, rather than general optical devices such as lenses, etc. that could operate under a classical theory of light. The laser is an extremely important application and is discussed above under stimulated emission.

Individual photons can be detected by several methods. The classic photomultiplier tube exploits the photoelectric effect: a photon of sufficient energy strikes a metal plate and knocks free an electron, initiating an ever-amplifying avalanche of electrons. Semiconductor charge-coupled device chips use a similar effect: an incident photon generates a charge on a microscopic capacitor that can be detected. Other detectors such as Geiger counters use the ability of photons to ionize gas molecules contained in the device, causing a detectable change of conductivity of the gas.^{ [114] }

Planck's energy formula is often used by engineers and chemists in design, both to compute the change in energy resulting from a photon absorption and to determine the frequency of the light emitted from a given photon emission. For example, the emission spectrum of a gas-discharge lamp can be altered by filling it with (mixtures of) gases with different electronic energy level configurations.^{ [115] }

Under some conditions, an energy transition can be excited by "two" photons that individually would be insufficient. This allows for higher resolution microscopy, because the sample absorbs energy only in the spectrum where two beams of different colors overlap significantly, which can be made much smaller than the excitation volume of a single beam (see two-photon excitation microscopy). Moreover, these photons cause less damage to the sample, since they are of lower energy.^{ [116] }

In some cases, two energy transitions can be coupled so that, as one system absorbs a photon, another nearby system "steals" its energy and re-emits a photon of a different frequency. This is the basis of fluorescence resonance energy transfer, a technique that is used in molecular biology to study the interaction of suitable proteins.^{ [117] }

Several different kinds of hardware random number generators involve the detection of single photons. In one example, for each bit in the random sequence that is to be produced, a photon is sent to a beam-splitter. In such a situation, there are two possible outcomes of equal probability. The actual outcome is used to determine whether the next bit in the sequence is "0" or "1".^{ [118] }^{ [119] }

Much research has been devoted to applications of photons in the field of quantum optics. Photons seem well-suited to be elements of an extremely fast quantum computer, and the quantum entanglement of photons is a focus of research. Nonlinear optical processes are another active research area, with topics such as two-photon absorption, self-phase modulation, modulational instability and optical parametric oscillators. However, such processes generally do not require the assumption of photons *per se*; they may often be modeled by treating atoms as nonlinear oscillators. The nonlinear process of spontaneous parametric down conversion is often used to produce single-photon states. Finally, photons are essential in some aspects of optical communication, especially for quantum cryptography.^{ [lower-alpha 8] }

Two-photon physics studies interactions between photons, which are rare. In 2018, MIT researchers announced the discovery of bound photon triplets, which may involve polaritons.^{ [120] }^{ [121] }

- Advanced Photon Source at Argonne National Laboratory
- Ballistic photon
- Dirac equation
- Doppler effect
- EPR paradox
- High energy X-ray imaging technology
- Luminiferous aether
- Medipix
- Phonon
- Photography
- Photon counting
- Photon energy
- Photon epoch
- Photon polarization
- Photonic molecule
- Photonics
- Single-photon source
- Spin angular momentum of light
- Static forces and virtual-particle exchange

- ↑ The photon's invariant mass (also called "rest mass" for massive particles) is believed to be exactly zero. This is the notion of particle mass generally used by modern physicists. The photon does have a nonzero relativistic mass, depending on its energy, but this varies according to the frame of reference.
- ↑ Although the 1967 Elsevier translation of Planck's Nobel Lecture interprets Planck's
*Lichtquant*as "photon", the more literal 1922 translation by Hans Thacher Clarke and Ludwik Silberstein Planck, Max (1922).*The Origin and Development of the Quantum Theory*. Clarendon Press. (here) uses "light-quantum". No evidence is known that Planck himself used the term "photon" by 1926 (see also). - ↑ Isaac Asimov credits Arthur Compton with defining quanta of energy as photons in 1923.
^{ [12] } - ↑ The mass of the photon is believed to be exactly zero. Some sources also refer to the
*relativistic mass*, which is just the energy scaled to units of mass. For a photon with wavelength*λ*or energy*E*, this is*h*/*λc*or*E*/*c*^{2}. This usage for the term "mass" is no longer common in scientific literature. Further info: What is the mass of a photon? - ↑ The phrase "no matter how intense" refers to intensities below approximately 10
^{13}W/cm^{2}at which point perturbation theory begins to break down. In contrast, in the intense regime, which for visible light is above approximately 10^{14}W/cm^{2}, the classical wave description correctly predicts the energy acquired by electrons, called ponderomotive energy. (See also: Boreham, Bruce W.; Hora, Heinrich; Bolton, Paul R. (1996). "Photon density and the correspondence principle of electromagnetic interaction".*AIP Conference Proceedings*.**369**: 1234–1243. Bibcode:1996AIPC..369.1234B. doi:10.1063/1.50410.) By comparison, sunlight is only about 0.1 W/cm^{2}. - ↑ These experiments produce results that cannot be explained by any classical theory of light, since they involve anticorrelations that result from the quantum measurement process. In 1974, the first such experiment was carried out by Clauser, who reported a violation of a classical Cauchy–Schwarz inequality. In 1977, Kimble
*et al.*demonstrated an analogous anti-bunching effect of photons interacting with a beam splitter; this approach was simplified and sources of error eliminated in the photon-anticorrelation experiment of Grangier*et al.*(1986). This work is reviewed and simplified further in Thorn*et al.*(2004). (These references are listed below.) - ↑ The issue was first formulated by Theodore Duddell Newton and Eugene Wigner.
^{ [63] }^{ [64] }^{ [65] }The challenges arise from the fundamental nature of the Lorentz group, which describes the symmetries of spacetime in special relativity. Unlike the generators of Galilean transformations, the generators of Lorentz boosts do not commute, and so simultaneously assigning low uncertainties to all coordinates of a relativistic particle's position becomes problematic.^{ [66] } - ↑ Introductory-level material on the various sub-fields of quantum optics can be found in Fox, M. (2006).
*Quantum Optics: An Introduction*. Oxford University Press. ISBN 978-0-19-856673-1.

In atomic physics, the **Bohr model** or **Rutherford–Bohr model**, presented by Niels Bohr and Ernest Rutherford in 1913, is a system consisting of a small, dense nucleus surrounded by orbiting electrons—similar to the structure of the Solar System, but with attraction provided by electrostatic forces in place of gravity. After the cubic model (1902), the plum-pudding model (1904), the Saturnian model (1904), and the Rutherford model (1911) came the *Rutherford–Bohr model* or just *Bohr model* for short (1913). The improvement to the Rutherford model is mostly a quantum physical interpretation of it. The model's key success lay in explaining the Rydberg formula for the spectral emission lines of atomic hydrogen. While the Rydberg formula had been known experimentally, it did not gain a theoretical underpinning until the Bohr model was introduced. Not only did the Bohr model explain the reasons for the structure of the Rydberg formula, it also provided a justification for the fundamental physical constants that make up the formula's empirical results.

In physics, **electromagnetic radiation** refers to the waves of the electromagnetic field, propagating (radiating) through space, carrying electromagnetic radiant energy. It includes radio waves, microwaves, infrared, (visible) light, ultraviolet, X-rays, and gamma rays.

The **photoelectric effect** is the emission of electrons when electromagnetic radiation, such as light, hits a material. Electrons emitted in this manner are called photoelectrons. The phenomenon is studied in condensed matter physics, and solid state and quantum chemistry to draw inferences about the properties of atoms, molecules and solids. The effect has found use in electronic devices specialized for light detection and precisely timed electron emission.

**Quantum mechanics** is a fundamental theory in physics that provides a description of the physical properties of nature at the scale of atoms and subatomic particles. It is the foundation of all quantum physics including quantum chemistry, quantum field theory, quantum technology, and quantum information science.

**Wave–particle duality** is the concept in quantum mechanics that every particle or quantum entity may be described as either a particle or a wave. It expresses the inability of the classical concepts "particle" or "wave" to fully describe the behaviour of quantum-scale objects. As Albert Einstein wrote:

It seems as though we must use sometimes the one theory and sometimes the other, while at times we may use either. We are faced with a new kind of difficulty. We have two contradictory pictures of reality; separately neither of them fully explains the phenomena of light, but together they do.

**Radiation pressure** is the mechanical pressure exerted upon any surface due to the exchange of momentum between the object and the electromagnetic field. This includes the momentum of light or electromagnetic radiation of any wavelength which is absorbed, reflected, or otherwise emitted by matter on any scale. The associated force is called the **radiation pressure force**, or sometimes just the **force of light**.

**Atomic, molecular, and optical physics** (**AMO**) is the study of matter-matter and light-matter interactions; at the scale of one or a few atoms and energy scales around several electron volts. The three areas are closely interrelated. AMO theory includes classical, semi-classical and quantum treatments. Typically, the theory and applications of emission, absorption, scattering of electromagnetic radiation (light) from excited atoms and molecules, analysis of spectroscopy, generation of lasers and masers, and the optical properties of matter in general, fall into these categories.

In the physical sciences, the **wavenumber** is the spatial frequency of a wave, measured in cycles per unit distance or radians per unit distance. Whereas temporal frequency can be thought of as the number of waves per unit time, wavenumber is the number of waves per unit distance.

**Planck's law** describes the spectral density of electromagnetic radiation emitted by a black body in thermal equilibrium at a given temperature *T*, when there is no net flow of matter or energy between the body and its environment.

**Matter waves** are a central part of the theory of quantum mechanics, being an example of wave–particle duality. All matter exhibits wave-like behavior. For example, a beam of electrons can be diffracted just like a beam of light or a water wave. In most cases, however, the wavelength is too small to have a practical impact on day-to-day activities. Hence in our day-to-day lives with objects the size of tennis balls and people, matter waves are not relevant.

The **old quantum theory** is a collection of results from the years 1900–1925 which predate modern quantum mechanics. The theory was never complete or self-consistent, but was rather a set of heuristic corrections to classical mechanics. The theory is now understood as the semi-classical approximation to modern quantum mechanics.

The **Abraham–Minkowski controversy** is a physics debate concerning electromagnetic momentum within dielectric media. Traditionally, it is argued that in the presence of matter the electromagnetic stress-energy tensor by itself is not conserved (divergenceless). Only the total stress-energy tensor carries unambiguous physical significance, and how one apportions it between an "electromagnetic" part and a "matter" part depends on context and convenience. In other words, the electromagnetic part and the matter part in the total momentum can be arbitrarily distributed as long as the total momentum is kept the same. There are two incompatible equations to describe momentum transfer between matter and electromagnetic fields. These two equations were first suggested by Hermann Minkowski (1908) and Max Abraham (1909), from which the controversy's name derives. Both were claimed to be supported by experimental data. Theoretically, it is usually argued that Abraham's version of momentum "does indeed represent the true momentum density of electromagnetic fields" for electromagnetic waves, while Minkowski's version of momentum is "pseudomomentum" or "wave momentum".

**Einstein coefficients** are mathematical quantities which are a measure of the probability of absorption or emission of light by an atom or molecule. The Einstein *A* coefficients are related to the rate of spontaneous emission of light, and the Einstein *B* coefficients are related to the absorption and stimulated emission of light.

**Quantum mechanics** is the science of the very small. It explains the behavior of matter and its interactions with energy on the scale of atomic and subatomic particles. By contrast, classical physics explains matter and energy only on a scale familiar to human experience, including the behavior of astronomical bodies such as the Moon. Classical physics is still used in much of modern science and technology. However, towards the end of the 19th century, scientists discovered phenomena in both the large (macro) and the small (micro) worlds that classical physics could not explain. The desire to resolve inconsistencies between observed phenomena and classical theory led to two major revolutions in physics that created a shift in the original scientific paradigm: the *theory of relativity* and the development of *quantum mechanics*. This article describes how physicists discovered the limitations of classical physics and developed the main concepts of the quantum theory that replaced it in the early decades of the 20th century. It describes these concepts in roughly the order in which they were first discovered. For a more complete history of the subject, see *History of quantum mechanics*.

The **history of quantum mechanics** is a fundamental part of the history of modern physics. Quantum mechanics' history, as it interlaces with the history of quantum chemistry, began essentially with a number of different scientific discoveries: the 1838 discovery of cathode rays by Michael Faraday; the 1859–60 winter statement of the black-body radiation problem by Gustav Kirchhoff; the 1877 suggestion by Ludwig Boltzmann that the energy states of a physical system could be *discrete*; the discovery of the photoelectric effect by Heinrich Hertz in 1887; and the 1900 quantum hypothesis by Max Planck that any energy-radiating atomic system can theoretically be divided into a number of discrete "energy elements" *ε* such that each of these energy elements is proportional to the frequency *ν* with which each of them individually radiate energy, as defined by the following formula:

The **Planck constant**, or **Planck's constant**, is the quantum of electromagnetic action that relates a photon's energy to its frequency. The Planck constant multiplied by a photon's frequency is equal to a photon's energy. The Planck constant is a fundamental physical constant denoted as , and of fundamental importance in quantum mechanics. In metrology it is used to define the kilogram in SI units.

**Photoelectrochemical processes** are processes in photoelectrochemistry; they usually involve transforming light into other forms of energy. These processes apply to photochemistry, optically pumped lasers, sensitized solar cells, luminescence, and photochromism.

The **Planck–Einstein relation** is also referred to as the **Einstein relation**, **Planck's energy–frequency relation**, the **Planck relation**, and the **Planck equation**. Also the **Planck formula** belongs on this list, but also often refers to Planck's law instead. These various eponyms are far from standard; they are used only sporadically, neither regularly nor very widely. They refer to a formula integral to quantum mechanics, which states that the energy of a photon, *E*, known as photon energy, is proportional to its frequency, *ν*:

In 1922, American physicist William Duane presented a discrete momentum-exchange model of the reflection of X-Ray photons by a crystal lattice. Duane showed that such a model gives the same scattering angles as the ones calculated via a wave diffraction model, see Bragg's Law.

A hallmark of Albert Einstein's career was his use of visualized thought experiments as a fundamental tool for understanding physical issues and for elucidating his concepts to others. **Einstein's thought experiments** took diverse forms. In his youth, he mentally chased beams of light. For special relativity, he employed moving trains and flashes of lightning to explain his most penetrating insights. For general relativity, he considered a person falling off a roof, accelerating elevators, blind beetles crawling on curved surfaces and the like. In his debates with Niels Bohr on the nature of reality, he proposed imaginary devices intended to show, at least in concept, how the Heisenberg uncertainty principle might be evaded. In a profound contribution to the literature on quantum mechanics, Einstein considered two particles briefly interacting and then flying apart so that their states are correlated, anticipating the phenomenon known as quantum entanglement.

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*Newsweek*. Retrieved 17 February 2018. - ↑ Liang, Qi-Yu; et al. (16 February 2018). "Observation of three-photon bound states in a quantum nonlinear medium".
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By date of publication:

- Alonso, M.; Finn, E.J. (1968).
*Fundamental University Physics Volume III: Quantum and Statistical Physics*. Addison-Wesley. ISBN 978-0-201-00262-1.CS1 maint: ref=harv (link) - Clauser, J.F. (1974). "Experimental distinction between the quantum and classical field-theoretic predictions for the photoelectric effect".
*Physical Review D*.**9**(4): 853–860. Bibcode:1974PhRvD...9..853C. doi:10.1103/PhysRevD.9.853. - Pais, A. (1982).
*Subtle is the Lord: The Science and the Life of Albert Einstein*. Oxford University Press. - Feynman, Richard (1985).
*QED: The Strange Theory of Light and Matter*. Princeton University Press. ISBN 978-0-691-12575-6. - Grangier, P.; Roger, G.; Aspect, A. (1986). "Experimental Evidence for a Photon Anticorrelation Effect on a Beam Splitter: A New Light on Single-Photon Interferences".
*Europhysics Letters*.**1**(4): 173–179. Bibcode:1986EL......1..173G. CiteSeerX 10.1.1.178.4356 . doi:10.1209/0295-5075/1/4/004. - Lamb, W.E. (1995). "Anti-photon".
*Applied Physics B*.**60**(2–3): 77–84. Bibcode:1995ApPhB..60...77L. doi:10.1007/BF01135846. - Special supplemental issue of
*Optics and Photonics News*(vol. 14, October 2003) article web link- Roychoudhuri, C.; Rajarshi, R. (2003). "The nature of light: what is a photon?".
*Optics and Photonics News*.**14**: S1 (Supplement). - Zajonc, A. "Light reconsidered".
*Optics and Photonics News*.**14**: S2–S5 (Supplement). - Loudon, R. "What is a photon?".
*Optics and Photonics News*.**14**: S6–S11 (Supplement). - Finkelstein, D. "What is a photon?".
*Optics and Photonics News*.**14**: S12–S17 (Supplement). - Muthukrishnan, A.; Scully, M.O.; Zubairy, M.S. "The concept of the photon – revisited".
*Optics and Photonics News*.**14**: S18–S27 (Supplement). - Mack, H.; Schleich, W.P. "A photon viewed from Wigner phase space".
*Optics and Photonics News*.**14**: S28–S35 (Supplement).

- Roychoudhuri, C.; Rajarshi, R. (2003). "The nature of light: what is a photon?".
- Glauber, R. (2005). "One Hundred Years of Light Quanta" (PDF).
*2005 Physics Nobel Prize Lecture*. Archived from the original (PDF) on 2008-07-23. Retrieved 2009-06-29. - Hentschel, K. (2007). "Light quanta: The maturing of a concept by the stepwise accretion of meaning".
*Physics and Philosophy*.**1**(2): 1–20.

Education with single photons:

- Thorn, J.J.; Neel, M.S.; Donato, V.W.; Bergreen, G.S.; Davies, R.E.; Beck, M. (2004). "Observing the quantum behavior of light in an undergraduate laboratory" (PDF).
*American Journal of Physics*.**72**(9): 1210–1219. Bibcode:2004AmJPh..72.1210T. doi:10.1119/1.1737397. - Bronner, P.; Strunz, Andreas; Silberhorn, Christine; Meyn, Jan-Peter (2009). "Interactive screen experiments with single photons".
*European Journal of Physics*.**30**(2): 345–353. Bibcode:2009EJPh...30..345B. doi:10.1088/0143-0807/30/2/014.

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