In quantum physics, a quantum fluctuation (or vacuum state fluctuation or vacuum fluctuation) is the temporary random change in the amount of energy in a point in space,[2] as prescribed by Werner Heisenberg's uncertainty principle. They are tiny random fluctuations in the values of the fields which represent elementary particles, such as electric and magnetic fields which represent the electromagnetic force carried by photons, W and Z fields which carry the weak force, and gluon fields which carry the strong force.[3] Vacuum fluctuations appear as virtual particles, which are always created in particle-antiparticle pairs.[4] Since they are created spontaneously without a source of energy, vacuum fluctuations and virtual particles are said to violate the conservation of energy. This is theoretically allowable because the particles annihilate each other within a time limit determined by the uncertainty principle so they are not directly observable.[4][3] The uncertainty principlestates the uncertainty in energy and time can be related by[5] , where
12ħ ≈ 5,27286×10−35 Js. This means that pairs of virtual particles with energy and lifetime shorter than are continually created and annihilated in empty space. Although the particles are not directly detectable, the cumulative effects of these particles are measurable. For example, without quantum fluctuations the "bare" mass and charge of elementary particles would be infinite; from renormalization theory the shielding effect of the cloud of virtual particles is responsible for the finite mass and charge of elementary particles. Another consequence is the Casimir effect. One of the first observations which was evidence for vacuum fluctuations was the Lamb shift in hydrogen. In July 2020, scientists reported that quantum vacuum fluctuations can influence the motion of macroscopic, human-scale objects by measuring correlations below the standard quantum limitbetween the position/momentum uncertainty of the mirrors of LIGO and the photon number/phase uncertainty of light that they reflect.[6][7][8]
https://en.wikipedia.org/wiki/Quantum_fluctuation
https://en.wikipedia.org/wiki/Quantum_annealing
https://en.wikipedia.org/wiki/Quantum_foam
The cosmic microwave background (CMB, CMBR), in Big Bang cosmology, is electromagnetic radiation which is a remnant from an early stage of the universe, also known as "relic radiation".[1] The CMB is faint cosmic background radiation filling all space. It is an important source of data on the early universe because it is the oldest electromagnetic radiation in the universe, dating to the epoch of recombination. With a traditional optical telescope, the space between stars and galaxies (the background) is completely dark. However, a sufficiently sensitive radio telescope shows a faint background noise, or glow, almost isotropic, that is not associated with any star, galaxy, or other object. This glow is strongest in the microwave region of the radio spectrum. The accidental discovery of the CMBin 1965 by American radio astronomers Arno Penzias and Robert Wilson[2][3] was the culmination of work initiated in the 1940s, and earned the discoverers the 1978 Nobel Prize in Physics.
https://en.wikipedia.org/wiki/Cosmic_microwave_background
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