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	== Further reading ==		== Further reading ==

	*{{Cite book \|last=Longair \|first=Malcolm S. ~~\|url=https://www.worldcat.org/oclc/702125055~~ \|title=High energy astrophysics \|date=2011 \|publisher=Cambridge University Press \|isbn=978-0-511-93059-1 \|edition=3rd \|location=Cambridge \|oclc=702125055}}		*{{Cite book \|last=Longair \|first=Malcolm S. \|title=High energy astrophysics \|date=2011 \|publisher=Cambridge University Press \|isbn=978-0-511-93059-1 \|edition=3rd \|location=Cambridge \|oclc=702125055}}
	*{{Cite book \|last=Rybicki \|first=George B. \|url=https://www.bartol.udel.edu/~owocki/phys633/RadProc-RybLightman.pdf \|title=Radiative processes in astrophysics \|date=2004 \|others=Alan P. Lightman \|isbn=978-3-527-61817-0 \|location=Weinheim \|pages=191 \|oclc=212140606}}		*{{Cite book \|last=Rybicki \|first=George B. \|url=https://www.bartol.udel.edu/~owocki/phys633/RadProc-RybLightman.pdf \|title=Radiative processes in astrophysics \|date=2004 \|others=Alan P. Lightman \|isbn=978-3-527-61817-0 \|location=Weinheim \|pages=191 \|oclc=212140606}}

	[[Category:Special functions]]		[[Category:Special functions]]

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2023-11-07T05:22:32Z

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[[Image:Synchrotron Functions.svg|thumb|First and second Synchrotron functions.]]
In [[mathematics]] the '''synchrotron functions''' are defined as follows (for ''x'' ≥ 0):<ref>{{Cite journal |last1=Fouka |first1=M. |last2=Ouichaoui |first2=S. |date=2013-01-29 |title=Analytical Fits to the Synchrotron Functions |journal=Research in Astronomy and Astrophysics |volume=13 |issue=6 |pages=680–686 |language=en |doi=10.1088/1674-4527/13/6/007|arxiv=1301.6908 |bibcode=2013RAA....13..680F |s2cid=118480582 }}</ref>

* First synchrotron function <math display="block">F(x) = x \int_x^\infty K_{\frac{5}{3}}(t)\,dt</math>
* Second synchrotron function <math display="block">G(x) = x K_{\frac{2}{3}}(x)</math>

where ''K''<sub>''j''</sub> is the modified [[Bessel function]] of the second kind.

== Use in astrophysics ==

In [[astrophysics]], x is usually a ratio of frequencies, that is, the frequency over a critical frequency (critical frequency is the frequency at which most [[synchrotron radiation]] is radiated). This is needed when calculating the spectra for different types of synchrotron emission. It takes a spectrum of electrons (or any charged particle) generated by a separate process (such as a power law distribution of electrons and positrons from a constant injection spectrum) and converts this to the spectrum of photons generated by the input electrons/positrons.

== References ==
<references />

== Further reading ==

*{{Cite book |last=Longair |first=Malcolm S. |url=https://www.worldcat.org/oclc/702125055 |title=High energy astrophysics |date=2011 |publisher=Cambridge University Press |isbn=978-0-511-93059-1 |edition=3rd |location=Cambridge |oclc=702125055}}
*{{Cite book |last=Rybicki |first=George B. |url=https://www.bartol.udel.edu/~owocki/phys633/RadProc-RybLightman.pdf |title=Radiative processes in astrophysics |date=2004 |others=Alan P. Lightman |isbn=978-3-527-61817-0 |location=Weinheim |pages=191 |oclc=212140606}}

[[Category:Special functions]]

Synchrotron function - Revision history

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