Physics:Quantum noise

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Quantum noise is a type of noise in a quantum system due to quantum mechanical phenomena such as quantized fields and the uncertainty principle. This principle says that some observables cannot simultaneously be known with arbitrary precision. This indeterminate state of matter introduces a fluctuation in the value of properties of a quantum system, even at zero temperature. These fluctuations in the absence of thermal noise are known as zero-point energy fluctuations.

Quantum noise can also come from the discrete nature of the small quantum constituents such as electrons and quantum effects, such as photocurrents. An example of this form of quantum noise is shot noise as coined by J. Verdeyen which comes from the discrete arrival of photons or electrons in a detector. Because these quanta arrive randomly in time, even a perfectly steady current or light beam exhibits fluctuations in the detected signal.

In most systems, classical noise dominates over quantum noise, because classical fluctuations are several orders of magnitude larger, and it masks the effects of quantum noise. Quantum noise generally only becomes visible after suppressing the effects of conventional noise sources such as thermal fluctuations, mechanical vibrations, and industrial noise by cooling a system to a millikelvin range and using extremely low-noise electronics. This is why quantum noise is present in superconducting circuits and in the LIGO gravitational wave observatory, but not in many conventional settings.

At absolute zero temperature, classical noise vanishes. However, unlike classical noise, quantum noise cannot be completely eliminated as it arises directly from fundamental tenets of quantum mechanics. The uncertainty principle requires any amplifier or detector to have some noise, setting a fundamental limit on the accuracy of these instruments. Despite this fact, experimental physicists still define an "ideal" amplifier or detector as one that optimizes the fundamental quantum noise inequality, known as a "quantum-limited detector".

Noise is of practical concern for precision engineering and engineered systems approaching the standard quantum limit. Typical engineered consideration of quantum noise is for quantum nondemolition measurement and quantum point contact. So quantifying noise is useful.

The term "quantum noise" is often used in the fields of quantum information and quantum computing as an umbrella term for unwanted environmental disturbances that affect quantum systems and cause decoherence. An isolated quantum system, such as a qubit, has a state that will evolve deterministically. But in an open system, such as those found in nature, the qubit interacts with uncontrolled degrees of freedom in its environment, introducing fluctuations which are commonly referred to as quantum noise. This is distinct from the above definition, which specifically concerns intrinsic noise due to the nature of quantum mechanics, not all environmental sources of noise and decoherence. In practice, however, definitions of quantum noise often include environmental or external disturbances affecting quantum systems.

noise in the Quantum Collection.

Principles

Noise theory

A signal's noise is quantified as the Fourier transform of its autocorrelation. The autocorrelation of a signal is given as $$G_{vv}(t-t^{\prime })=⟨V(t)V(t^{\prime })⟩,$$ which measures when our signal is positively, negatively or not correlated at different times $t$ and $t^{\prime }$. The time average, $⟨V(t)⟩$, is zero and our $V(t)$ is a voltage signal. Its Fourier transform is $$V(\omega )=\frac{1}{\sqrt{T}}\underset{0}{\overset{T}{\int }}V(t)e^{i\omega t}dt$$ because we measure a voltage over a finite time window. The Wiener–Khinchin theorem generally states that a noise's power spectrum is given as the autocorrelation of a signal, i.e., $$S_{vv}(\omega )=\underset{-\mathrm{\infty }}{\overset{+\mathrm{\infty }}{\int }}{e}^{i\omega t}{G}_{vv}dt=\underset{-\mathrm{\infty }}{\overset{+\mathrm{\infty }}{\int }}{e}^{i\omega t}⟨|V(\omega ){|}^2⟩dt$$The above relation is sometimes called the power spectrum or spectral density. In the above outline, we assumed that

• Our noise is stationary or the probability does not change over time. Only the time difference matters.
• Noise is due to a very large number of fluctuating charge so that the central limit theorem applied, i.e., the noise is Gaussian or normally distributed.
• $G_{vv}$ decays to zero rapidly over some time ${\tau }_c$.
• We sample over a sufficiently large time, $T$, that our integral scales as a random walk $\sqrt{T}$. So our $V(\omega )$ is independent of measured time for $T\gg {\tau }_c$. Said in another way, $G_{vv}(t-t^{\prime })\to 0$ as $|t-t^{\prime }|\gg {\tau }_c$.

One can show that an ideal "top-hat" signal, which may correspond to a finite measurement of a voltage over some time, will produce noise across its entire spectrum as a sinc function. Even in the classical case, noise is produced.

Classical to quantum noise

To study quantum noise, one replaces the corresponding classical measurements with quantum operators, e.g., $$S_{xx}(\omega )=\underset{-\mathrm{\infty }}{\overset{+\mathrm{\infty }}{\int }}{e}^{i\omega t}⟨\hat{x}(t)\hat{x}(0)⟩dt,$$ where $⟨\cdot ⟩$ are the quantum statistical average using the density matrix in the Heisenberg picture.

Heisenberg microscope

Quantum noise can be illustrated by considering a Heisenberg microscope where an atom's position is measured from the scattering of photons. The uncertainty principle is given as,

$$\mathrm{\Delta }{x}_{imp}\mathrm{\Delta }{p}_{BA}\gtrsim \hslash .$$

Where the $\mathrm{\Delta }{x}_{imp}$ is the uncertainty in an atom's position, and the $\mathrm{\Delta }{p}_{BA}$ is the uncertainty of the momentum or sometimes called the backaction (momentum transferred to the atom) when near the quantum limit. The precision of the position measurement can be increased at the expense of knowing the atom's momentum. When the position is precisely known enough backaction begins to affect the measurement in two ways. First, it will impart momentum back onto the measuring devices in extreme cases. Secondly, we have decreasing future knowledge of the atom's future position. Precise and sensitive instrumentation will approach the uncertainty principle at sufficiently control environments.

Heisenberg uncertainty and noise

The Heisenberg uncertainty implies the existence of noise. An operator with a hermitian conjugate follows the relationship, $A{A}^{†}\ge 0$. Define $A$ as $A=\delta x+\lambda e^{i\theta }\delta y$ where $\lambda$ is real. The $x$ and $y$ are the quantum operators. We can show the following,

$$⟨\delta x^2⟩⟨\delta y^2⟩\ge \frac{1}{4}|⟨[\delta x,\delta y]⟩{|}^2+|⟨[\delta x,\delta y{]}_{+}⟩{|}^2$$ where the $⟨\cdot ⟩$ are the averages over the wavefunction and other statistical properties. The left terms are the uncertainty in $x$ and $y$, the second term on the right is to covariance or $⟨\delta x\delta y+\delta y\delta x⟩$ which arises from coupling to an external source or quantum effects. The first term on the right corresponds to the Commutator relation and would cancel out if the x and y commuted. That is the origin of our quantum noise.

It is demonstrative to let $x$ and $y$ correspond to position and momentum that meets the well known commutator relation, $[x,p]=i\hslash$. Then our new expression is,

$$\mathrm{\Delta }x\mathrm{\Delta }y\ge \sqrt{\frac{1}{4}{\hslash }^2+{\sigma }_{xy}^2}$$

Where the ${\sigma }_{xy}$ is the correlation. If the second term on the right vanishes, then we recover the Heisenberg uncertainty principle.

Harmonic motion and weakly coupled heat bath

Consider the motion of a simple harmonic oscillator with mass, $M$, and frequency, $\mathrm{\Omega }$, coupled to some heat bath which keeps the system in equilibrium. The equations of motion are given as,

$$x(t)=x(0)\cos (\mathrm{\Omega }t)+p(0)\frac{1}{M\mathrm{\Omega }}\sin (\mathrm{\Omega }t)$$

The quantum autocorrelation is then,

$$\begin{array}{rl}{G}_{xx}& =⟨\hat{x}(t)\hat{x}(0)⟩\\ & =⟨\hat{x}(0)\hat{x}(0)⟩\cos (\mathrm{\Omega }t)+⟨\hat{p}(0)\hat{x}(0)⟩\sin (\mathrm{\Omega }t)\end{array}$$

Classically, there is no correlation between position and momentum. The uncertainty principle requires the second term to be nonzero. It goes to $i\hslash /2$. We can take the equipartition theorem or the fact that in equilibrium the energy is equally shared among a molecule/atoms degrees of freedom in thermal equilibrium, i.e.,

$$\frac{1}{2}M{\mathrm{\Omega }}^2⟨x^2⟩=\frac{1}{2}{k}_{\text{B}}T$$

In the classical autocorrelation, we have

$$G_{xx}=\frac{k_{\text{B}}T}{M{\mathrm{\Omega }}^2}\cos (\mathrm{\Omega }t)\to S_{xx}(\omega )=\pi \frac{k_{\text{B}}T}{M{\mathrm{\Omega }}^2}[\delta (\omega -\mathrm{\Omega })+\delta (\omega +\mathrm{\Omega })]$$

while in the quantum autocorrelation we have

$$G_{xx}=\left(\frac{\hslash }{2M\mathrm{\Omega }}\right)\{n_{BE}(\hslash \mathrm{\Omega })e^{i\mathrm{\Omega }t}+[n_{BE}(\hslash \mathrm{\Omega })+1]e^{-i\mathrm{\Omega }t}\}\to S_{xx}(\omega )=2\pi \left(\frac{\hslash }{2M\mathrm{\Omega }}\right)[n_{BE}(\hslash \mathrm{\Omega })\delta (\omega -\mathrm{\Omega })+[n_{BE}(\hslash \mathrm{\Omega })+1]\delta (\omega +\mathrm{\Omega })]$$

Where the fraction terms in parentheses is the zero-point energy uncertainty. The $n_{BE}$ is the Bose-Einstein population distribution. Notice that the quantum $S_{xx}$ is asymmetric in the due to the imaginary autocorrelation. As we increase to higher temperature that corresponds to taking the limit of $k_{B}T\gg \hslash \mathrm{\Omega }$. One can show that the quantum approaches the classical $S_{xx}$. This allows $n_{BE}\approx n_{BE}+1\approx \frac{k_{\text{B}}T}{\hslash \mathrm{\Omega }}$

Physical interpretation of spectral density

Typically, the positive frequency of the spectral density corresponds to the flow of energy into the oscillator (for example, the photons' quantized field), while the negative frequency corresponds to the emitted of energy from the oscillator. Physically, an asymmetric spectral density would correspond to either the net flow of energy from or to our oscillator model.

Linear gain and quantum uncertainty

Most optical communications use amplitude modulation where the quantum noise is predominantly the shot noise. A laser's quantum noise, when not considering shot noise, is the uncertainty of its electric field's amplitude and phase. That uncertainty becomes observable when a quantum amplifier preserves phase. The phase noise becomes important when the energy of the frequency modulation or phase modulation is comparable to the energy of the signal (frequency modulation is more robust than amplitude modulation due to the additive noise intrinsic to amplitude modulation).

Linear amplification

An ideal noiseless gain cannot exit. Consider the amplification of stream of photons, an ideal linear noiseless gain, and the Energy-Time uncertainty relation.

$$\mathrm{\Delta }E\mathrm{\Delta }t\gtrsim \hslash /2$$

The photons, ignoring the uncertainty in frequency, will have an uncertainty in its overall phase and number, and assume a known frequency, i.e., $\mathrm{\Delta }\varphi =2\pi \nu \mathrm{\Delta }t$ and $\mathrm{\Delta }E=h\nu \mathrm{\Delta }n$. We can substitute these relations into our energy-time uncertainty equation to find the number-phase uncertainty relation or the uncertainty in the phase and photon numbers. $$\mathrm{\Delta }n\mathrm{\Delta }\varphi >1/2$$

Let an ideal linear noiseless gain, $G$, act on the photon stream. We also assume a unity quantum efficiency, or every photon is converted to a photocurrent. The output will be following with no noise added.

$$n_0\pm \mathrm{\Delta }{n}_0\to G{n}_0\pm G\mathrm{\Delta }{n}_0$$

The phase will be modified too,

$${\varphi }_0\pm \mathrm{\Delta }{\varphi }_0\to {\varphi }_0+\theta +\mathrm{\Delta }{\varphi }_0,$$ where the $\theta$ is the overall accumulated phase as the photons traveled through the gain medium. Substituting our output gain and phase uncertainties, gives us $$\mathrm{\Delta }{n}_0\mathrm{\Delta }{\varphi }_0>1/2G.$$

Our gain is $G>1$, which is a contradiction to our uncertainty principles. So a linear noiseless amplifier cannot increase its signal without noise. A deeper analysis done by H. Heffner showed the minimum noise power output required to meet the Heisenberg uncertainty principle is given as $$P_n=h\nu B(G-1)$$ where $B$ is half of the full width at half max, the $\nu$ frequency of the photons, and $h$ is the Planck constant. The term $h\nu B_0/2$ with $B_0=2B$ is sometimes called quantum noise

Types of Quantum Noise

Shot noise

In precision optics with highly stabilized lasers and efficient detectors, quantum noise refers to the fluctuations of signal.

The random error of interferometric measurements of position, due to the discrete character of photons measurement, is another quantum noise. The uncertainty of position of a probe in probe microscopy may also attributable to quantum noise; but not the dominant mechanism governing resolution.

In an electric circuit, the random fluctuations of a signal due to the discrete character of electrons can be called quantum noise.

An experiment by S. Saraf, et .al. demonstrated shot noise limited measurements as a demonstration of quantum noise measurements. Generally speaking, they amplified a Nd:YAG free space laser with minimal noise addition as it transitioned from linear to nonlinear amplification. The experiment required Fabry-Perot for filtering laser mode noises and selecting frequencies, two separate but identical probe and saturating beams to ensure uncorrelated beams, a zigzag slab gain medium, and a balanced detector for measuring quantum noise or shot-noise limited noise.

Shot Noise Power

The theory behind noise analysis of photon statistics (sometimes called the forward Kolmogorov equation) starts from the Masters equation from Shimoda et al.

$$\frac{d{P}_n}{dx}=a[n{P}_{n-1}-(n+1)P_n]+b[(n+1)P_{n+1}-n{P}_n]$$

where $a$ corresponds to the emission cross section and upper population number product ${\sigma }_e{N}_2$, and the $b$ is the absorption cross section ${\sigma }_a{N}_1$. The above relation is describing the probability of finding $n$ photons in radiation mode $|n⟩$. The dynamic only considers neighboring modes $|n+1⟩$ and $|n-1⟩$ as the photons travel through a medium of excited and ground state atoms from position $x$ to $x+dx$. This gives us a total of 4 photon transitions associated to one photon energy level. Two photon number adding to the field and leaving an atom, $|n-1⟩\to |n⟩$ and $|n⟩\to |n+1⟩$ and two photons leaving a field to the atom $|n+1⟩\to |n⟩$ and $|n⟩\to |n-1⟩$. Its noise power is given as,

$$P_d^2=P_{\text{shot}}^2[1+2f_{sp}\eta (G-1)]$$

Where,

• $P_d$ is the power at the detector,
• $P_{\text{shot}}$ is the power limited shot noise,
• $G$ the unsaturated gain and is also true for saturated gain,
• $\eta$ is the efficiency factor. That is the product of transmission window efficiency to our photodetector, and quantum efficiency.
• $f_{sp}$ is the spontaneous emission factor that typically corresponds relative strength of spontaneous emission to stimulated emission. A value of unity would mean all doped ions are in the excited state.

Sarif, et al. demonstrated quantum noise or shot noise limited measurements over a wide range of power gain that agreed with theory.

Quantum Back Action

Back action is the phenomenon in which the act of measuring a property of a particle directly influences the state of the particle.

In quantum mechanics, operators which do not commute are considered incompatible observables, and carry an associated uncertainty principle:

${\sigma }_x{\sigma }_p\ge \hslash /2$

When measuring these observables, this principle sets a minimum uncertainty in their values.

Each observable operator has a set of eigenstates. The initial state of a system, described by the wavefunction, is a linear combination of the full set of its eigenstates. Once measured, the system's wavefunction collapses to an eigenstate of that observable. It will then evolve in time again. Because the act of measurement altered the state of the observable, it affects the future behavior and any future measurement of the system. This introduces error, and is the concept behind back action.

Back action is a practical source of noise in experiments. Whenever a probe or measurement device interacts with a system, through photons, electrons, or other carriers, ithe measurement process imparts a random disturbance. In precision instruments, this disturbance appears as an additional noise source that limits sensitivity, known as measurement back-action noise.

Experimental setups involving optical measurement are limited by both shot noise and backaction noise. In an optomechanical system such as a laser interferometer, measurement back-action noise arises because of fluctuations in the radiation pressure of the light. By increasing the optical power, the shot noise is decreased, but this comes at the cost of increasing backaction, in the form of quantum radiation pressure noise, and the backaction of the randomly-arriving photons’ radiation pressure will become the dominant force on the system.

Vacuum Fluctuations / Zero-Point Noise

The existence of zero-point energy fluctuations is well-established in the theory of the quantised electromagnetic field. Generally speaking, at the lowest energy excitation of a quantized field that permeates all space (i.e. the field mode being in the vacuum state), the root-mean-square fluctuation of field strength is non-zero. This accounts for vacuum fluctuations that permeate all space.

This vacuum fluctuation or quantum noise will effect classical systems. This manifest as quantum decoherence in an entangled system, normally attributed to thermal differences in the conditions surrounding each entangled particle. Because entanglement is studied intensely in simple pairs of entangled photons, for example, decoherence observed in experiments could well be synonymous with "quantum noise" as to the source of the decoherence. Vacuum fluctuation is a possible causes for a quanta of energy to spontaneously appear in a given field or spacetime, then thermal differences must be associated with this event. Hence, it would cause decoherence in an entangled system in proximity of the event.

Quantum amplifiers

A laser is described by the coherent state of light, or the superposition of harmonic oscillators eigenstates. Erwin Schrödinger first derived the coherent state for the Schrödinger equation to meet the correspondence principle in 1926.

The laser is a quantum mechanical phenomena (see Maxwell–Bloch equations, rotating wave approximation, and semi-classical model of a two level atom). The Einstein coefficients and the laser rate equations are adequate if one is interested in the population levels and one does not need to account for population quantum coherences (the off diagonal terms in a density matrix). Photons of the order of 10⁸ corresponds to a moderate energy. The relative error of measurement of the intensity due to the quantum noise is on the order of 10⁻⁵. This is considered to be of good precision for most of applications.

A quantum amplifier is an amplifier which operates close to the quantum limit. Quantum noise becomes important when a small signal is amplified. A small signal's quantum uncertainties in its quadrature are also amplified; this sets a lower limit to the amplifier. A quantum amplifier's noise is its output amplitude and phase. Generally, a laser is amplified across a spread of wavelengths around a central wavelength, some mode distribution, and polarization spread. But one can consider a single mode amplification and generalize to many different modes. A phase-invariant amplifier preserves the phase of the input gain without drastic changes to the output phase mode.

Quantum amplification can be represented with a unitary operator, $A_{\text{out}}=U^{†}{A}_{\text{in}}U$ , as stated in D. Kouznetsov 1995 paper.

Applications

Experimental suppression using reflective boundaries

A study published in Physical Review Research (2025) by scientists at Swansea University demonstrated a novel method of suppressing quantum noise using reflective boundaries. By placing a nanoparticle at the focal center of a hemispherical mirror, researchers found that the particle became indistinguishable from its mirror image under specific conditions. This configuration prevented extraction of positional information from scattered light, which in turn eliminated the associated quantum backaction, the disturbance caused by measurement using photons.

This counterintuitive effect occurred precisely when light scattering was maximized, suggesting a fundamental link between information availability and quantum noise. The study opened avenues for highly sensitive quantum sensors, macroscopic quantum state experiments, and applications in space-based quantum physics missions such as MAQRO (Macroscopic Quantum Resonators).

Index

Core theory

1. Foundations

2. Conceptual and interpretations

3. Mathematical structure and systems

4. Atomic and spectroscopy

5. Wavefunctions and modes

6. Quantum dynamics and evolution

7. Measurement and information

8. Quantum information and computing

Applications and extensions

9. Quantum optics and experiments

10. Open quantum systems

11. Quantum field theory

12. Statistical mechanics and kinetic theory

13. Condensed matter and solid-state physics

14. Plasma and fusion physics

15. Timeline

16. Advanced and frontier topics

Book II

• Matter by scale

Book III

• Methods and tools

Book IV

• Data Analysis Techniques

Full contents

1. Foundations (14) Back to index

1. Physics:Quantum basics

2. Physics:Quantum photoelectric effect

3. Physics:Quantum black-body radiation

4. Physics:Quantum Planck constant

5. Physics:Quantum Postulates

6. Physics:Quantum Hilbert space

7. Physics:Quantum Observables and operators

8. Physics:Quantum mechanics

9. Physics:Quantum mechanics measurements

10. Physics:Quantum state

11. Physics:Quantum system

12. Physics:Quantum superposition

13. Physics:Quantum probability

14. Physics:Quantum Mathematical Foundations of Quantum Theory

2. Conceptual and interpretations (14) Back to index

15. Physics:Quantum Interpretations of quantum mechanics

16. Physics:Quantum Wave–particle duality

17. Physics:Quantum Complementarity principle

18. Physics:Quantum Uncertainty principle

19. Physics:Quantum Measurement problem

20. Physics:Quantum Bell's theorem

21. Physics:Quantum Hidden variable theory

22. Physics:Quantum nonlocality

23. Physics:Quantum contextuality

24. Physics:Quantum Darwinism

25. Physics:Quantum A Spooky Action at a Distance

26. Physics:Quantum A Walk Through the Universe

27. Physics:Quantum The Secret of Cohesion and How Waves Hold Matter Together

28. Physics:Quantum measurement problem

3. Mathematical structure and systems (15) Back to index

29. Physics:Quantum Density matrix

30. Physics:Quantum Exactly solvable quantum systems

31. Physics:Quantum many-body problem

32. Physics:Quantum Formulas Collection

33. Physics:Quantum A Matter Of Size

34. Physics:Quantum Symmetry in quantum mechanics

35. Physics:Quantum Noether theorem

36. Physics:Quantum Angular momentum operator

37. Physics:Quantum Runge–Lenz vector

38. Physics:Quantum Approximation Methods

39. Physics:Quantum Matter Elements and Particles

40. Physics:Quantum Dirac equation

41. Physics:Quantum Klein–Gordon equation

42. Physics:Quantum pendulum

43. Physics:Quantum configuration space

4. Atomic and spectroscopy (14) Back to index

44. Physics:Quantum Atomic structure and spectroscopy

45. Physics:Quantum Hydrogen atom

46. Physics:Quantum number

47. Physics:Quantum Multi-electron atoms

48. Physics:Quantum Fine structure

49. Physics:Quantum Hyperfine structure

50. Physics:Quantum Isotopic shift

51. Physics:Quantum defect

52. Physics:Quantum Zeeman effect

53. Physics:Quantum Stark effect

54. Physics:Quantum Spectral lines and series

55. Physics:Quantum Selection rules

56. Physics:Quantum Fermi's golden rule

57. Physics:Quantum beats

5. Wavefunctions and modes (9) Back to index

58. Physics:Quantum Wavefunction

59. Physics:Quantum Superposition principle

60. Physics:Quantum Eigenstates and eigenvalues

61. Physics:Quantum Boundary conditions and quantization

62. Physics:Quantum Standing waves and modes

63. Physics:Quantum Normal modes and field quantization

64. Physics:Number of independent spatial modes in a spherical volume

65. Physics:Quantum Density of states

66. Physics:Quantum carpet

6. Quantum dynamics and evolution (21) Back to index

67. Physics:Quantum Time evolution

68. Physics:Quantum Schrödinger equation

69. Physics:Quantum Time-dependent Schrödinger equation

70. Physics:Quantum Stationary states

71. Physics:Quantum Perturbation theory

72. Physics:Quantum Time-dependent perturbation theory

73. Physics:Quantum Adiabatic theorem

74. Physics:Quantum Berry phase

75. Physics:Quantum Aharonov-Bohm effect

76. Physics:Quantum Aharonov-Casher effect

77. Physics:Quantum Scattering theory

78. Physics:Quantum Scattering matrix

79. Physics:Quantum S-matrix

80. Physics:Quantum tunnelling

81. Physics:Quantum speed limit

82. Physics:Quantum revival

83. Physics:Quantum reflection

84. Physics:Quantum oscillations

85. Physics:Quantum jump

86. Physics:Quantum boomerang effect

87. Physics:Quantum chaos

7. Measurement and information (9) Back to index

88. Physics:Quantum Measurement theory

89. Physics:Quantum Measurement operators

90. Physics:Quantum Projective measurement

91. Physics:Quantum POVM

92. Physics:Quantum Weak measurement

93. Physics:Quantum Measurement collapse

94. Physics:Quantum entanglement

95. Physics:Quantum Zeno effect

96. Physics:Quantum limit

8. Quantum information and computing (15) Back to index

97. Physics:Quantum information theory

98. Physics:Quantum Qubit

99. Physics:Quantum Entanglement

100. Physics:Quantum Bell state

101. Physics:Quantum Gates and circuits

102. Physics:Quantum BB84

103. Physics:Quantum No-cloning theorem

104. Physics:Quantum Computing Algorithms in the NISQ Era

105. Physics:Quantum Noisy Qubits

106. Physics:Quantum error correction

107. Physics:Quantum Boson sampling

108. Physics:Quantum random access code

109. Physics:Quantum pseudo-telepathy

110. Physics:Quantum network

111. Physics:Quantum money

9. Quantum optics and experiments (10) Back to index

112. Physics:Quantum Nonlinear King plot anomaly in calcium isotope spectroscopy

113. Physics:Quantum Stern-Gerlach experiment

114. Physics:Quantum Experimental quantum physics

115. Physics:Quantum optics

116. Physics:Quantum optics beam splitter experiments

117. Physics:Quantum Mach-Zehnder interferometer

118. Physics:Quantum Hong-Ou-Mandel effect

119. Physics:Quantum eraser experiment

120. Physics:Quantum delayed-choice quantum eraser

121. Physics:Quantum Ultra fast lasers

122. Template:Quantum optics operators

10. Open quantum systems (15) Back to index

123. Physics:Quantum Open systems

124. Physics:Quantum channel

125. Physics:Quantum Kraus operators

126. Physics:Quantum Amplitude damping

127. Physics:Quantum Phase damping

128. Physics:Quantum Depolarizing channel

129. Physics:Quantum Master equation

130. Physics:Quantum Lindblad equation

131. Physics:Quantum Decoherence

132. Physics:Quantum Dynamical decoupling

133. Physics:Quantum dissipation

134. Physics:Quantum Markov semigroup

135. Physics:Quantum Markovian dynamics

136. Physics:Quantum Non-Markovian dynamics

137. Physics:Quantum Trajectories

11. Quantum field theory (23) Back to index

138. Physics:Quantum field theory (QFT) basics

139. Physics:Quantum field theory (QFT) core

140. Physics:Quantum Fields and Particles

141. Physics:Quantum Second quantization

142. Physics:Quantum Fock space

143. Physics:Quantum Harmonic Oscillator field modes

144. Physics:Quantum Creation and annihilation operators

145. Physics:Quantum vacuum fluctuations

146. Physics:Quantum Casimir effect

147. Physics:Quantum Propagators in quantum field theory

148. Physics:Quantum Feynman diagrams

149. Physics:Quantum Path integral formulation

150. Physics:Quantum Renormalization in field theory

151. Physics:Quantum Renormalization group

152. Physics:Quantum Field Theory Gauge symmetry

153. Physics:Quantum Spontaneous symmetry breaking

154. Physics:Quantum Non-Abelian gauge theory

155. Physics:Quantum Electrodynamics (QED)

156. Physics:Quantum chromodynamics (QCD)

157. Physics:Quantum Electroweak theory

158. Physics:Quantum Standard Model

159. Physics:Quantum triviality

160. Physics:Quantum confinement problem

12. Statistical mechanics and kinetic theory (9) Back to index

161. Physics:Quantum Statistical mechanics

162. Physics:Quantum Partition function

163. Physics:Quantum Distribution functions

164. Physics:Quantum Liouville equation

165. Physics:Quantum Kinetic theory

166. Physics:Quantum Boltzmann equation

167. Physics:Quantum BBGKY hierarchy

168. Physics:Quantum Relaxation and thermalization

169. Physics:Quantum Thermodynamics

13. Condensed matter and solid-state physics (17) Back to index

170. Physics:Quantum Band structure

171. Physics:Quantum Fermi surfaces

172. Physics:Quantum Landau levels

173. Physics:Quantum fractional Hall effect

174. Physics:Quantum Semiconductor physics

175. Physics:Quantum Phonons

176. Physics:Quantum Electron-phonon interaction

177. Physics:Quantum Exchange interaction

178. Physics:Quantum Superconductivity

179. Physics:Quantum Topological phases of matter

180. Physics:Quantum anyon

181. Physics:Quantum well

182. Physics:Quantum spin liquid

183. Physics:Quantum spin Hall effect

184. Physics:Quantum phase transition

185. Physics:Quantum critical point

186. Physics:Quantum dot

14. Plasma and fusion physics (8) Back to index

187. Physics:Quantum Fusion reactions and Lawson criterion

188. Physics:Quantum Plasma (fusion context)

189. Physics:Quantum Magnetic confinement fusion

190. Physics:Quantum Inertial confinement fusion

191. Physics:Quantum Plasma instabilities and turbulence

192. Physics:Quantum Tokamak core plasma

193. Physics:Quantum Tokamak edge physics and recycling asymmetries

194. Physics:Quantum Stellarator

15. Timeline (8) Back to index

195. Physics:Quantum mechanics/Timeline

196. Physics:Quantum mechanics/Timeline/Pre-quantum era

197. Physics:Quantum mechanics/Timeline/Old quantum theory

198. Physics:Quantum mechanics/Timeline/Modern quantum mechanics

199. Physics:Quantum mechanics/Timeline/Quantum field theory era

200. Physics:Quantum mechanics/Timeline/Quantum information era

201. Physics:Quantum mechanics/Timeline/Quantum technology era

202. Physics:Quantum mechanics/Timeline/Quiz

16. Advanced and frontier topics (16) Back to index

203. Physics:Quantum topology

204. Physics:Quantum battery

205. Physics:Quantum Supersymmetry

206. Physics:Quantum Black hole thermodynamics

207. Physics:Quantum Holographic principle

208. Physics:Quantum gravity

209. Physics:Quantum De Sitter invariant special relativity

210. Physics:Quantum Doubly special relativity

211. Physics:Quantum arithmetic geometry

212. Physics:Quantum unsolved problems

213. Physics:Quantum Yang-Mills mass gap

214. Physics:Quantum gravity problem

215. Physics:Quantum black hole information paradox

216. Physics:Quantum dark matter problem

217. Physics:Quantum neutrino mass problem

218. Physics:Quantum matter-antimatter asymmetry problem

References

Sources

• Clark, Aashish A. (2008). "Quantum Noise and quantum measurement". Oxford University Press. https://clerkgroup.uchicago.edu/PDFfiles/LesHouchesNotesAC.pdf. 
• Clerk, A. A.; Devoret, M. H.; Girvin, S. M.; Marquardt, Florian; Schoelkopf, R. J. (2010). "Introduction to quantum noise, measurement, and amplification". Reviews of Modern Physics 82 (2): 1155–1208. doi:10.1103/RevModPhys.82.1155. Bibcode: 2010RvMP...82.1155C. 
• Gardiner, Crispin W.; Zoller, Peter (2004). Quantum Noise: A Handbook of Markovian and Non-Markovian Quantum Stochastic Methods with Applications to Quantum Optics (3rd ed.). Berlin ; Heidelberg: Springer. ISBN 978-3-540-22301-6. https://books.google.com/books?id=a_xsT8oGhdgC. 

Source attribution: Quantum noise