Vela Pulsar

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Vela Pulsar
Vela Pulsar jet.jpg
The Vela Pulsar and its surrounding pulsar wind nebula, Chandra X-Ray image
Observation data
Epoch J2000      Equinox J2000
Constellation Vela
Right ascension 08h 35m 20.65525s
Declination −45° 10′ 35.1545″[1]
Apparent magnitude (V) 23.6
Astrometry
Distance 959 (-163,+248) ly
(294 (-50,+76)[2] pc)
Other designations
PSR B0833-45, 4U 0833-45, 2CG 263-02, 2E 0833.6-4500, 3EG J0834-4511, H 0833-450, INTEGRAL1 5, SNR G263.6-02.8

The Vela Pulsar (PSR B0833-45 or PSR J0835-4510) is a radio, optical, X-ray and gamma-emitting pulsar associated with the Vela Supernova Remnant in the constellation of Vela.

Supernova origins[edit]

The association of the Vela pulsar with the Vela Supernova Remnant, made by astronomers at the University of Sydney in 1968,[3] was direct observational proof that supernovae form neutron stars.

Characteristics[edit]

It has a period of 89 milliseconds (the shortest known at the time of its discovery) and the remnant from the supernova explosion is estimated to be travelling outwards at 1,200 km/s (750 mi/s).[4] It has the third brightest optical component of all known pulsars (V = 23.6 mag)[5] which pulses twice for every single radio pulse. The Vela pulsar is the brightest persistent object in the high energy gamma ray sky.

Vela X[edit]

The pulsar is occasional referred to as Vela X, but this is a separate phenomena. A radio survey of the Vela-Puppis region was made with the Mills Cross Telescope in 1956-57 and identified three strong radio sources: Vela X, Vela Y, and Vela Z. These sources are close to the entirely separate Puppis A supernova remnant, which is also a strong X-ray and radio source.[6]

Studies conducted by Kellogg et al. with the Uhuru spacecraft in 1970-71 showed Vela X and the Vela pulsar to be separate but spatially related objects. The term "Vela X" was used to describe the entirety of the supernova remnant.[7] Weiler and Panagia established in 1980 that Vela X was actually a pulsar wind nebula, contained within the fainter supernova remnant and driven by energy released by the pulsar.[8]

Neither the pulsar nor either of the associated nebulae should be confused with Vela X-1, a nearby but unrelated high-mass X-ray binary system.

Gallery[edit]

References[edit]

  1. ^ "Vela pulsar". SIMBAD. Retrieved 9 January 2013. 
  2. ^ Caraveo, P. A.; De Luca, A.; Mignani, R. P.; Bignami, G. F. (November 2001). "The Distance to the Vela Pulsar Gauged with Hubble Space Telescope Parallax Observations". Astrophys. J. 561 (2): 930–937. arXiv:astro-ph/0107282. Bibcode:2001ApJ...561..930C. doi:10.1086/323377. 
  3. ^ Large, M. I.; Vaughan, A. E.; Mills, B. Y. (October 1968). "A Pulsar Supernova Association?". Nature 20 (5165): 340–341. Bibcode:1968Natur.220..340L. doi:10.1038/220340a0. 
  4. ^ Lyne, Andrew G.; Graham-Smith, Francis (1998). Pulsar Astronomy (2nd ed.). Cambridge University Press. ISBN 0-521-59413-8. 
  5. ^ Mignani, R. P.; Zharikov, R. P.; Caraveo, P. A. (October 2007). "The Optical Spectrum of the Vela Pulsar". Astronomy and Astrophysics 473 (3): 891. arXiv:0707.2036. Bibcode:2007A&A...473..891M. doi:10.1051/0004-6361:20077774. 
  6. ^ Rishbeth, H. (December 1958). "Radio Emission from the Vela-Puppis Region". Australian Journal of Physics 11 (4): 550–563. Bibcode:1958AuJPh..11..550R. doi:10.1071/PH580550. 
  7. ^ Kellogg, E.; Tananbaum, H.; Harnden, F. R., Jr.; Gursky, H.; Giacconi, R.; Grindlay, J. (August 1973). "The X-ray Structure of the Vela X Region Observed from Uhuru". The Astrophysical Journal 183: 935–940. Bibcode:1973ApJ...183..935K. doi:10.1086/152279. 
  8. ^ 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. 

External links[edit]


Coordinates: Sky map 08h 35m 20.65525s, −45° 10′ 35.1545″