Editing Synchrotron radiation (section)

===In supernovae===
When a star explodes in a supernova, the fastest ejecta move at semi-relativistic speeds approximately 10% the [[speed of light]].<ref>{{cite journal |last1=Soderberg |first1=A. |author1-link= Alicia M. Soderberg |last2=Chevalier |first2=R. A. |last3=Kulkarni |first3=S. R. |last4=Frail |first4=D. A. |date=November 2006 |title=The Radio and X-Ray Luminous SN 2003bg and the Circumstellar Density Variations around Radio Supernovae |journal=The Astrophysical Journal |volume=651 |issue=2 |pages=1005–1018 |doi=10.1086/507571|doi-access=free |arxiv=astro-ph/0512413 |bibcode=2006ApJ...651.1005S }}</ref> This blast wave gyrates electrons in ambient magnetic fields and generates synchrotron emission, revealing the radius of the blast wave at the location of the emission.<ref>{{cite journal |last1=Chevalier |first1=R. A. |date=May 1998 |title=Synchrotron Self-Absorption in Radio Supernovae |journal=The Astrophysical Journal |volume=499 |issue=2 |pages=810–819 |doi=10.1086/305676|doi-access=free |bibcode=1998ApJ...499..810C }}</ref> Synchrotron emission can also reveal the strength of the magnetic field at the front of the shock wave, as well as the circumstellar density it encounters, but strongly depends on the choice of energy partition between the magnetic field, proton kinetic energy, and electron kinetic energy. Radio synchrotron emission has allowed astronomers to shed light on mass loss and stellar winds that occur just prior to stellar death.<ref>{{cite journal |last1=Margutti |first1=Raffaella |last2=Kamble |first2=A. |last3=Milisavljevic |first3=D. |last4=Zapartas |first4=E. |last5=de Mink |first5=S. E. |last6=Drout |first6=M. |last7=Chornock |first7=R. |display-authors=1 |date=February 2017 |title=Ejection of the Massive Hydrogen-rich Envelope Timed with the Collapse of the Stripped SN 2014C |journal=The Astrophysical Journal |volume=835 |issue=2 |page=140 |doi=10.3847/1538-4357/835/2/140|hdl=10150/624387 |hdl-access=free |doi-access=free |pmid=28684881 |pmc=5495200 |arxiv=1601.06806 |bibcode=2017ApJ...835..140M }}</ref><ref>{{cite journal |last1=DeMarchi |first1=Lindsay |last2=Margutti |first2=R. |last3=Dittman |first3=J. |last4=Brunthaler |first4=A. |display-authors=1 |date=October 2022 |title=Radio Analysis of SN2004C Reveals an Unusual CSM Density Profile as a Harbinger of Core Collapse |journal=The Astrophysical Journal |volume=938 |issue=1 |page=84 |doi=10.3847/1538-4357/ac8c26|doi-access=free |arxiv=2203.07388 |bibcode=2022ApJ...938...84D }}</ref>