Editing Pulsar wind nebula (section)

{{Short description|Nebula powered by the pulsar wind of a pulsar}}
[[Image:Vela Pulsar jet.jpg|thumb|The [[Vela Pulsar]] (centre) and its surrounding pulsar wind nebula]]
[[Image:Chandra-crab.jpg|thumb|The inner [[Crab Nebula]]. Central part shows the pulsar wind nebula, with the red star in the centre being the [[Crab Pulsar]]. Image combines optical data from [[Hubble Space Telescope|Hubble]] (in red) and [[X-ray astronomy|X-ray]] data from [[Chandra X-ray Observatory|Chandra]] (in blue).]]

A '''pulsar wind nebula''' ('''PWN''', plural '''PWNe'''), sometimes called a '''plerion''' (derived from the Greek "πλήρης", ''pleres'', meaning "full"),<ref name="Weiler1978">{{cite journal |title=Are Crab-type Supernova Remnants (Plerions) Short-lived? |journal=Astronomy & Astrophysics |first1=K. W. |last1=Weiler |first2=N. |last2=Panagia |volume=70 |pages=419–422 |date=November 1978 |bibcode=1978A&A....70..419W}}</ref> is a type of [[nebula]] sometimes found inside the shell of a [[supernova remnant]] (SNR), powered by winds generated by a central [[pulsar]]. These nebulae were proposed as a class in 1976 as enhancements at [[radio wave]]lengths inside supernova remnants.<ref name="Weiler1978" /> They have since been found to be [[infrared]], optical, millimetre, [[X-ray]]<ref name="SafiHarb2012">{{cite conference |title=Plerionic supernova remnants |conference=AIP Conference Proceedings: 5th International Meeting on High Energy Gamma-Ray Astronomy |first=Samar |last=Safi-Harb |series=AIP Conference Proceedings |volume=1505 |pages=13–20 |date=December 2012 |doi=10.1063/1.4772215 |bibcode=2012AIPC.1505...13S |arxiv=1210.5406|s2cid=119113738 }}</ref> and [[gamma ray]] sources.<ref name="Guetta2003">{{cite journal |title=Observational implications of a plerionic environment for gamma-ray bursts |journal=Monthly Notices of the Royal Astronomical Society |first1=Dafne |last1=Guetta |first2=Jonathan |last2=Granot |volume=340 |issue=1 |pages=115–138 |date=March 2003 |doi=10.1046/j.1365-8711.2003.06296.x |doi-access=free |bibcode=2003MNRAS.340..115G |arxiv=astro-ph/0208156|s2cid=14308769 }}</ref><ref name="Gaensler2006" />