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Relativistic Breit–Wigner distribution

From Wikipedia, the free encyclopedia

The relativistic Breit–Wigner distribution (after the 1936 nuclear resonance formula[1] of Gregory Breit and Eugene Wigner) is a continuous probability distribution with the following probability density function,[2]

where k is a constant of proportionality, equal to


(This equation is written using natural units, ħ = c = 1.)

It is most often used to model resonances (unstable particles) in high-energy physics. In this case, E is the center-of-mass energy that produces the resonance, M is the mass of the resonance, and Γ is the resonance width (or  decay width), related to its mean lifetime according to τ = 1/Γ. (With units included, the formula is τ = ħ.)

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The probability of producing the resonance at a given energy E is proportional to f (E), so that a plot of the production rate of the unstable particle as a function of energy traces out the shape of the relativistic Breit–Wigner distribution. Note that for values of E off the maximum at M such that |E2 − M2| = MΓ, (hence |E − M| = Γ/2 for M ≫ Γ), the distribution f has attenuated to half its maximum value, which justifies the name for Γ, width at half-maximum.

In the limit of vanishing width, Γ → 0, the particle becomes stable as the Lorentzian distribution f sharpens infinitely to 2(E2 − M2).

In general, Γ can also be a function of E; this dependence is typically only important when Γ is not small compared to M and the phase space-dependence of the width needs to be taken into account. (For example, in the decay of the rho meson into a pair of pions.) The factor of M2 that multiplies Γ2 should also be replaced with E2 (or E 4/M2, etc.) when the resonance is wide.[3]

The form of the relativistic Breit–Wigner distribution arises from the propagator of an unstable particle,[4] which has a denominator of the form p2M2 + iMΓ. (Here, p2 is the square of the four-momentum carried by that particle in the tree Feynman diagram involved.) The propagator in its rest frame then is proportional to the quantum-mechanical amplitude for the decay utilized to reconstruct that resonance,

The resulting probability distribution is proportional to the absolute square of the amplitude, so then the above relativistic Breit–Wigner distribution for the probability density function.

The form of this distribution is similar to the amplitude of the solution to the classical equation of motion for a driven harmonic oscillator damped and driven by a sinusoidal external force. It has the standard resonance form of the Lorentz, or Cauchy distribution, but involves relativistic variables s = p2, here = E2. The distribution is the solution of the differential equation for the amplitude squared w.r.t. the energy energy (frequency), in such a classical forced oscillator,


Gaussian broadening

In experiment, the incident beam that produces resonance always has some spread of energy around a central value. Usually, that is a Gaussian/normal distribution. The resulting resonance shape in this case is given by the convolution of the Breit-Wigner and the Gaussian distribution,

This function can be simplified [5] by introducing new variables,

to obtain

where the relativistic line broadening function [5] has the following definition,

is the relativistic counterpart of the similar line-broadening function [6] for the Voigt profile used in spectroscopy (see also Section 7.19 of [7]).


  1. ^ Breit, G.; Wigner, E. (1936). "Capture of Slow Neutrons". Physical Review. 49 (7): 519. Bibcode:1936PhRv...49..519B. doi:10.1103/PhysRev.49.519.
  2. ^ See Pythia 6.4 Physics and Manual (page 98 onwards) for a discussion of the widths of particles in the PYTHIA manual. Note that this distribution is usually represented as a function of the squared energy.
  3. ^ Bohm, A.; Sato, Y. (2005). "Relativistic resonances: Their masses, widths, lifetimes, superposition, and causal evolution". Physical Review D. 71 (8). arXiv:hep-ph/0412106. Bibcode:2005PhRvD..71h5018B. doi:10.1103/PhysRevD.71.085018.
  4. ^ Brown, L S (1994). Quantum Field Theory, Cambridge University press, ISBN 978-0521469463 , Chapter 6.3.
  5. ^ a b Kycia, Radosław A.; Jadach, Stanisław (2018-07-15). "Relativistic Voigt profile for unstable particles in high energy physics". Journal of Mathematical Analysis and Applications. 463 (2): 1040–1051. arXiv:1711.09304. doi:10.1016/j.jmaa.2018.03.065. ISSN 0022-247X.
  6. ^ Finn, G. D.; Mugglestone, D. (1965-02-01). "Tables of the Line Broadening Function H ( a, υ )". Monthly Notices of the Royal Astronomical Society. 129 (2): 221–235. doi:10.1093/mnras/129.2.221. ISSN 0035-8711.
  7. ^ NIST handbook of mathematical functions. Olver, Frank W. J., 1924-, National Institute of Standards and Technology (U.S.). Cambridge: Cambridge University Press. 2010. ISBN 978-0-521-19225-5. OCLC 502037224.CS1 maint: others (link)
This page was last edited on 6 December 2020, at 19:52
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