The Vela Pulsar (centre) and its surrounding pulsar wind nebula
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 (in red) and X-ray data from Chandra (in blue).

A pulsar wind nebula (PWN, plural PWNe), sometimes called a plerion (derived from the Greek "πλήρης", pleres, meaning "full"),[1] 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 wavelengths inside supernova remnants.[1] They have since been found to be infrared, optical, millimetre, X-ray[2] and gamma ray sources.[3][4]

Evolution of pulsar wind nebulae

Pulsar wind nebulae evolve through various phases.[2][5] New pulsar wind nebulae appear soon after a pulsar's creation, and typically sit inside a supernova remnant, for example the Crab Nebula,[6] or the nebula within the large Vela Supernova Remnant.[7] As the pulsar wind nebula ages, the supernova remnant dissipates and disappears. Over time, pulsar wind nebulae may become bow-shock nebulae surrounding millisecond or slowly rotating pulsars.[8]

Properties of pulsar wind nebulae

Pulsar winds are composed of charged particles (plasma) accelerated to relativistic speeds by the rapidly rotating, hugely powerful magnetic fields above 1 teragauss (100 million teslas) 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 emission increases in the magnetized flow.

Pulsar wind nebulae often show the following properties:

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.[4]

See also


  1. ^ a b Weiler, K. W.; Panagia, N. (November 1978). "Are Crab-type Supernova Remnants (Plerions) Short-lived?". Astronomy & Astrophysics. 70: 419–422. Bibcode:1978A&A....70..419W.
  2. ^ a b Safi-Harb, Samar (December 2012). Plerionic supernova remnants. AIP Conference Proceedings: 5th International Meeting on High Energy Gamma-Ray Astronomy. AIP Conference Proceedings. Vol. 1505. pp. 13–20. arXiv:1210.5406. Bibcode:2012AIPC.1505...13S. doi:10.1063/1.4772215. S2CID 119113738.
  3. ^ Guetta, Dafne; Granot, Jonathan (March 2003). "Observational implications of a plerionic environment for gamma-ray bursts". Monthly Notices of the Royal Astronomical Society. 340 (1): 115–138. arXiv:astro-ph/0208156. Bibcode:2003MNRAS.340..115G. doi:10.1046/j.1365-8711.2003.06296.x. S2CID 14308769.
  4. ^ a b Gaensler, Bryan M.; Slane, Patrick O. (September 2006). "The Evolution and Structure of Pulsar Wind Nebulae". Annual Review of Astronomy and Astrophysics. 44 (1): 17–47. arXiv:astro-ph/0601081. Bibcode:2006ARA&A..44...17G. doi:10.1146/annurev.astro.44.051905.092528. S2CID 10699344.
  5. ^ a b Slane, Patrick O.; Chen, Yang; Schulz, Norbert S.; et al. (April 2000). "Chandra Observations of the Crab-like Supernova Remnant G21.5-0.9". Astrophysical Journal. 533 (1): L29–L32. arXiv:astro-ph/0001536. Bibcode:2000ApJ...533L..29S. doi:10.1086/312589. PMID 10727384. S2CID 17387448.
  6. ^ Hester, J. Jeff (September 2008). "The Crab Nebula: An Astrophysical Chimera". Annual Review of Astronomy & Astrophysics. 46 (1): 127–155. Bibcode:2008ARA&A..46..127H. doi:10.1146/annurev.astro.45.051806.110608.
  7. ^ Weiler, K. W.; Panagia, N. (October 1980). "Vela X and the Evolution of Plerions". Astronomy and Astrophysics. 90 (3): 269–282. Bibcode:1980A&A....90..269W.
  8. ^ Stappers, B. W.; Gaensler, B. M.; Kaspi, V. M.; et al. (February 2003). "An X-ray nebula associated with the millisecond pulsar B1957+20". Science. 299 (5611): 1372–1374. arXiv:astro-ph/0302588. Bibcode:2003Sci...299.1372S. doi:10.1126/science.1079841. PMID 12610299. S2CID 19659750.