Relativistic Breit–Wigner distribution

Template:Short description Template:Use dmy dates The relativistic Breit–Wigner distribution (after the 1936 nuclear resonance formula of Gregory Breit and Eugene Wigner) is a continuous probability distribution with the following probability density function,

$f(E)=\frac{k}{{(E^2-M^2)}^2+M^2{\mathrm{\Gamma }}^2},$

where Template:Mvar is a constant of proportionality, equal to

$k=\frac{2\sqrt{2}M\mathrm{\Gamma }\gamma }{\pi \sqrt{M^2+\gamma }}$ with $\gamma =\sqrt{M^2(M^2+{\mathrm{\Gamma }}^2)}.$

(This equation is written using natural units, Template:Nobr

It is most often used to model resonances (unstable particles) in high-energy physics. In this case, Template:Mvar is the center-of-mass energy that produces the resonance, Template:Mvar is the mass of the resonance, and Template:Math is the resonance width (or decay width), related to its mean lifetime according to Template:Nobr (With units included, the formula is Template:Nobr)

Usage

The probability of producing the resonance at a given energy Template:Mvar is proportional to Template:Math, 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 Template:Mvar off the maximum at Template:Mvar such that Template:Nobr (hence Template:Nobr for Template:Nobr the distribution Template:Mvar has attenuated to half its maximum value, which justifies the name for Template:Math, width at half-maximum.

In the limit of vanishing width, Template:Nobr the particle becomes stable as the Lorentzian distribution Template:Mvar sharpens infinitely to Template:Nobr where Template:Mvar is the Dirac delta function (point impulse).

In general, Template:Math can also be a function of Template:Mvar; this dependence is typically only important when Template:Math is not small compared to Template:Mvar 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 Template:Nobr that multipliesTemplate:Math should also be replaced with Template:Math (or Template:Nobr etc.) when the resonance is wide.

The form of the relativistic Breit–Wigner distribution arises from the propagator of an unstable particle, which has a denominator of the form Template:Nobr (Here, Template:Math 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,

$\frac{\sqrt{k}}{(E^2-M^2)+iM\mathrm{\Gamma }}.$

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 Template:Nobr here Template:Nobr 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,

$f^{\prime }(\mathrm{E})({({\mathrm{E}}^2-M^2)}^2+{\mathrm{\Gamma }}^2{M}^2)-4\mathrm{E}(M^2-{\mathrm{E}}^2)f(\mathrm{E})=0,$

or rather

$\frac{f^{\prime }(\mathrm{E})}{f(\mathrm{E})}=\frac{4(M^2-{\mathrm{E}}^2)\mathrm{E}}{{({\mathrm{E}}^2-M^2)}^2+{\mathrm{\Gamma }}^2{M}^2},$

with

$f(M)=\frac{k}{{\mathrm{\Gamma }}^2{M}^2}.$

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,

$V_2(E;M,\mathrm{\Gamma },k,\sigma )=\underset{-\mathrm{\infty }}{\overset{\mathrm{\infty }}{\int }}\frac{k}{(E{\text{'}}^2-M^2{)}^2+(M\mathrm{\Gamma }{)}^2}\frac{1}{\sigma \sqrt{2\pi }}{e}^{-\frac{(E^{\prime }-E{)}^2}{2{\sigma }^2}}\mathrm{d}{E}^{\prime }.$

This function can be simplified by introducing new variables,

$t=\frac{E-E^{\prime }}{\sqrt{2}\sigma },u_1=\frac{E-M}{\sqrt{2}\sigma },u_2=\frac{E+M}{\sqrt{2}\sigma },a=\frac{k\pi }{2{\sigma }^2},$

to obtain

$V_2(E;M,\mathrm{\Gamma },k,\sigma )=\frac{H_2(a,u_1,u_2)}{{\sigma }^{2}2\sqrt{\pi }},$

where the relativistic line broadening function has the following definition,

$H_2(a,u_1,u_2)=\frac{a}{\pi }\underset{-\mathrm{\infty }}{\overset{\mathrm{\infty }}{\int }}\frac{e^{-t^2}}{(u_1-t{)}^2(u_2-t{)}^2+a^2}\mathrm{d}t.$

$H_2$ is the relativistic counterpart of the similar line-broadening function for the Voigt profile used in spectroscopy (see also § 7.19 of ).