Holtsmark distribution

Holtsmark
Probability density function


Symmetric α-stable distributions with unit scale factor; α=1.5 (blue line) represents the Holtsmark distribution

Cumulative distribution function

Parameters

c ∈ (0, ∞) — scale parameter

μ ∈ (−∞, ∞) — location parameter
Support x ∈ R
PDF expressible in terms of hypergeometric functions; see text
Mean μ
Median μ
Mode μ
Variance infinite
Skewness undefined
Ex. kurtosis undefined
MGF undefined
CF \exp\left[~it\mu\!-\!|c t|^{3/2}~\right]

The (one-dimensional) Holtsmark distribution is a continuous probability distribution. The Holtsmark distribution is a special case of a stable distribution with the index of stability or shape parameter \alpha equal to 3/2 and skewness parameter \beta of zero. Since \beta equals zero, the distribution is symmetric, and thus an example of a symmetric alpha-stable distribution. The Holtsmark distribution is one of the few examples of a stable distribution for which a closed form expression of the probability density function is known. However, its probability density function is not expressible in terms of elementary functions; rather, the probability density function is expressed in terms of hypergeometric functions.

The Holtsmark distribution has applications in plasma physics and astrophysics.[1] In 1919, Norwegian physicist J. Holtsmark proposed the distribution as a model for the fluctuating fields in plasma due to chaotic motion of charged particles.[2] It is also applicable to other types of Coulomb forces, in particular to modeling of gravitating bodies, and thus is important in astrophysics.[3][4]

Characteristic function

The characteristic function of a symmetric stable distribution is:

\varphi(t;\mu,c) = \exp\left[~it\mu\!-\!|c t|^\alpha~\right],

where \alpha is the shape parameter, or index of stability, \mu is the location parameter, and c is the scale parameter.

Since the Holtsmark distribution has \alpha=3/2, its characteristic function is:[5]

\varphi(t;\mu,c) = \exp\left[~it\mu\!-\!|c t|^{3/2}~\right] .

Since the Holtsmark distribution is a stable distribution with α > 1, \mu represents the mean of the distribution.[6][7] Since β = 0, \mu also represents the median and mode of the distribution. And since α < 2, the variance of the Holtsmark distribution is infinite.[6] All higher moments of the distribution are also infinite.[6] Like other stable distributions (other than the normal distribution), since the variance is infinite the dispersion in the distribution is reflected by the scale parameter, c. An alternate approach to describing the dispersion of the distribution is through fractional moments.[6]

Probability density function

In general, the probability density function, f(x), of a continuous probability distribution can be derived from its characteristic function by:

f(x)=\frac{1}{2\pi}\int_{-\infty}^\infty \varphi(t)e^{-ixt}\,dt .

Most stable distributions do not have a known closed form expression for their probability density functions. Only the normal, Cauchy and Lévy distributions have known closed form expressions in terms of elementary functions.[1] The Holtsmark distribution is one of two symmetric stable distributions to have a known closed form expression in terms of hypergeometric functions.[1] When \mu is equal to 0 and the scale parameter is equal to 1, the Holtsmark distribution has the probability density function:

\begin{align} f(x; 0, 1) &= { 1 \over \pi } {\Gamma(5/3)} {}_2F_3(5/12,11/12;1/3,1/2,5/6;-4x^6/729) \\ & {} \quad{} - { x^2 \over 3\pi } {}_3F_4(3/4,1,5/4;2/3,5/6,7/6,4/3;-4x^6/729) \\ & {} \quad{} + { 7x^4 \over 81\pi } {\Gamma(4/3)} {}_2F_3(13/12,19/12;7/6,3/2,5/3;-4x^6/729) , \end{align}

where {\Gamma(x)} is the gamma function and \;_mF_n() is a hypergeometric function.[1]

References

  1. ↑ 1.0 1.1 1.2 1.3 Lee, W. H. (2010). Continuous and Discrete Properties of Stochastic Processes (PhD thesis). University of Nottingham. pp. 37–39.
  2. ↑ Holtsmark, J. (1919). "Uber die Verbreiterung von Spektrallinien". Annalen der Physik 363 (7): 577–630. Bibcode:1919AnP...363..577H. doi:10.1002/andp.19193630702.
  3. ↑ Chandrasekhar, S.; J. von Neumann (1942). "The Statistics of the Gravitational Field Arising from a Random Distribution of Stars. I. The Speed of Fluctuations". The Astrophysical Journal 95: 489. Bibcode:1942ApJ....95..489C. doi:10.1086/144420. ISSN 0004-637X. Retrieved 2011-03-01.
  4. ↑ Chandrasekhar, S. (1943-01-01). "Stochastic Problems in Physics and Astronomy". Reviews of Modern Physics 15 (1): 1. Bibcode:1943RvMP...15....1C. doi:10.1103/RevModPhys.15.1. Retrieved 2011-03-01.
  5. ↑ Zolotarev, V. M. (1986). One-Dimensional Stable Distributions. Providence, RI: American Mathematical Society. pp. 1, 41. ISBN 978-0-8218-4519-6.
  6. ↑ 6.0 6.1 6.2 6.3 Nolan, J. P. (2008). "Basic Properties of Univariate Stable Distributions". Stable Distributions: Models for Heavy Tailed Data. pp. 3, 15–16. Retrieved 2011-02-06.
  7. ↑ Nolan, J. P. (2003). "Modeling Financial Data". In Rachev, S. T. Handbook of Heavy Tailed Distributions in Finance. Amsterdam: Elsevier. pp. 111–112. ISBN 978-0-444-50896-6.