Editing Pulsar wind nebula

{{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" />

==Evolution of pulsar wind nebulae==

Pulsar wind nebulae evolve through various phases.<ref name="SafiHarb2012" /><ref name="Slane2000" /> New pulsar wind nebulae appear soon after a pulsar's creation, and typically sit inside a [[supernova remnant]], for example the [[Crab Nebula]],<ref name="Hester2008">{{cite journal |title=The Crab Nebula: An Astrophysical Chimera |journal=Annual Review of Astronomy & Astrophysics |first=J. Jeff |last=Hester |volume=46 |issue=1 |pages=127–155 |date=September 2008 |doi=10.1146/annurev.astro.45.051806.110608 |bibcode=2008ARA&A..46..127H}}</ref> or the nebula within the large [[Vela Supernova Remnant]].<ref name="Weiler1980">{{Cite journal |title=Vela X and the Evolution of Plerions |journal=[[Astronomy and Astrophysics]] |last1=Weiler |first1=K. W. |last2=Panagia |first2=N. |volume=90 |issue=3 |pages=269–282 |date=October 1980 |bibcode=1980A&A....90..269W}}</ref> As the pulsar wind nebula ages, the supernova remnant dissipates and disappears. Over time, pulsar wind nebulae may become [[Bow shock|bow-shock]] nebulae surrounding millisecond or slowly rotating pulsars.<ref name="Stappers2003">{{cite journal |title=An X-ray nebula associated with the millisecond pulsar B1957+20 |journal=Science |last1=Stappers |first1=B. W. |last2=Gaensler |first2=B. M. |last3=Kaspi |first3=V. M. |last4=van der Klis |first4=M. |last5=Lewin |first5=W. H. G. |display-authors=3 |volume=299 |issue=5611 |pages=1372–1374 |date=February 2003 |doi=10.1126/science.1079841 |arxiv=astro-ph/0302588 |bibcode=2003Sci...299.1372S |pmid=12610299|s2cid=19659750 }}</ref>

==Properties of pulsar wind nebulae==

Pulsar winds are composed of charged particles ([[plasma (physics)|plasma]]) accelerated to [[relativistic speed]]s by the rapidly rotating, powerful [[magnetic field]]s above {{convert|1|TG|e6T|abbr=off|lk=on}} that are generated by the spinning pulsar.  The pulsar wind often streams into the surrounding interstellar medium, creating a standing [[shock wave]] called the 'wind termination shock', where the wind decelerates to sub-relativistic speed. Beyond this radius, [[Synchrotron_radiation|synchrotron]] emission increases in the magnetized flow.

Pulsar wind nebulae often show the following properties:
* An increasing brightness towards the center, without a shell-like structure as seen in supernova remnants.
* A highly [[Polarization (waves)|polarized]] [[flux]] and a flat [[spectral index]] in the radio band, α=0–0.3. The index steepens at X-ray energies due to synchrotron radiation losses and on the average has an X-ray photon index of 1.3–2.3 (spectral index of 2.3–3.3).
* An X-ray size that is generally smaller than their radio and optical size (due to smaller synchrotron lifetimes of the higher-energy electrons).<ref name="Slane2000">{{cite journal |title=Chandra Observations of the Crab-like Supernova Remnant G21.5-0.9 |journal=Astrophysical Journal |first1=Patrick O. |last1=Slane |first2=Yang |last2=Chen |first3=Norbert S. |last3=Schulz |first4=Frederick D. |last4=Seward |first5=John P. |last5=Hughes |first6=Bryan M. |last6=Gaensler |display-authors=3 |volume=533 |issue=1 |pages=L29–L32 |date=April 2000 |pmid=10727384 |doi=10.1086/312589 |arxiv=astro-ph/0001536 |bibcode=2000ApJ...533L..29S|s2cid=17387448 }}</ref>
* A photon index at [[teraelectronvolt|TeV]] gamma-ray energies of ~2.3.

Pulsar wind nebulae can be powerful probes of a pulsar/neutron star's interaction with its surroundings. Their unique properties can be used to infer the geometry, energetics, and composition of the pulsar wind, the space velocity of the pulsar itself, and the properties of the ambient medium.<ref name="Gaensler2006">{{cite journal |title=The Evolution and Structure of Pulsar Wind Nebulae |journal=Annual Review of Astronomy and Astrophysics |last1=Gaensler |first1=Bryan M. |last2=Slane |first2=Patrick O. |volume=44 |issue=1 |pages=17–47 |date=September 2006 |doi=10.1146/annurev.astro.44.051905.092528 |arxiv=astro-ph/0601081 |bibcode=2006ARA&A..44...17G|s2cid=10699344 }}</ref>

==See also==
{{div col|colwidth=20em}}
* [[3C 58]]
* [[G292.0+01.8]]
*[[Crab Nebula]]
*[[Cosmic wind]]
*[[Stellar wind]]
*[[Solar wind]]
*[[Planetary wind]]
*[[Stellar-wind bubble]]
*[[Colliding-wind binary]]
*[[Galactic superwind]]
*[[Superwind]]
*[[Orders of magnitude (magnetic field)]]
{{div col end}}

==References==
{{Reflist}}

==External links==
* [http://www.physics.mcgill.ca/~pulsar/pwncat.html The Pulsar Wind Nebula Catalog]

{{Neutron star}}
{{Nebula}}

{{DEFAULTSORT:Pulsar Wind Nebula}}
[[Category:Pulsar wind nebulae| ]]
[[Category:Supernova remnants]]
[[Category:Pulsars|Wind nebula]]
[[Category:Nebulae]]
[[Category:Millisecond pulsars|Wind nebula]]