Editing Thomson scattering (section)

== Examples of Thomson scattering ==
[[File:Total Solar Eclipse 8-21-17.jpg|thumb|upright|right|Thomson scattering around the Sun visualizes the trajectory of charged particles in visible light.]]
The [[cosmic microwave background]] contains a small linearly-polarized component attributed to Thomson scattering. That polarized component mapping out the so-called [[cosmic microwave background#E-modes|E-modes]] was first detected by [[Degree Angular Scale Interferometer|DASI]] in 2002.

The solar [[K-corona]] is the result of the Thomson scattering of solar radiation from solar coronal electrons. The ESA and NASA [[Solar and Heliospheric Observatory|SOHO]] mission and the NASA [[STEREO]] mission generate three-dimensional images of the electron density around the Sun by measuring this K-corona from three separate satellites.

In [[tokamak]]s, corona of [[Inertial confinement fusion|ICF]] targets and other experimental [[fusion power|fusion]] devices, the electron temperatures and densities in the [[plasma (physics)|plasma]] can be [[plasma diagnostics#Thomson scattering|measured]] with high accuracy by detecting the effect of Thomson scattering of a high-intensity [[laser]] beam. An upgraded Thomson scattering system in the [[Wendelstein 7-X]] [[stellarator]] uses [[Nd:YAG lasers]] to emit multiple pulses in quick succession. The intervals within each burst can range from 2 ms to 33.3 ms, permitting up to twelve consecutive measurements. Synchronization with plasma events is made possible by a newly added trigger system that facilitates real-time analysis of transient plasma events.<ref>{{cite journal |last1=Damm |first1=H. |last2=Pasch |first2=E.  |last3=Dinklage |first3=A.  |last4=Baldzuhn |first4=J.|display-authors=3|title=First results from an event synchronized—high repetition Thomson scattering system at Wendelstein 7-X |journal=Journal of Instrumentation |date=2019 |volume=14 |issue=9 |pages=C09037 |doi=10.1088/1748-0221/14/09/C09037 |arxiv=1907.00492 |bibcode=2019JInst..14C9037D |s2cid=195767387 |url=https://iopscience.iop.org/article/10.1088/1748-0221/14/09/C09037 }}</ref>

In the [[Sunyaev–Zeldovich effect]], where the photon energy is much less than the electron rest mass, the [[Compton scattering|inverse-Compton scattering]] can be approximated as Thomson scattering in the rest frame of the electron.<ref>{{cite journal |last1=Birkinshaw |first1=Mark |title=The Sunyaev–Zel'dovich effect |journal=Physics Reports |date=1999 |volume=310 |issue=2–3 |pages=97–195 |doi=10.1016/s0370-1573(98)00080-5 |arxiv=astro-ph/9808050 |bibcode=1999PhR...310...97B |hdl=1983/5d24f14a-26e0-44d3-8496-5843b108fec5 |s2cid=119330362 |url=http://dx.doi.org/10.1016/S0370-1573(98)00080-5 |access-date=4 November 2021 }}</ref>

Models for [[X-ray crystallography]] are based on Thomson scattering.