Epoch J2000 Equinox J2000
|Right ascension||08h 35m 20.65525s|
|Declination||−45° 10′ 35.1545″|
|Apparent magnitude (V)||23.6|
|Distance||959 (-163,+248) ly
(294 (-50,+76) pc)
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). It has the third brightest optical component of all known pulsars (V = 23.6 mag) which pulses twice for every single radio pulse. The Vela pulsar is the brightest persistent object in the high energy gamma ray sky.
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.
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. 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.
Cycle of pulsed gamma rays from the Vela pulsar
- "Vela pulsar". SIMBAD. Retrieved 9 January 2013.
- 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.
- 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.
- Lyne, Andrew G.; Graham-Smith, Francis (1998). Pulsar Astronomy (2nd ed.). Cambridge University Press. ISBN 0-521-59413-8.
- 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.
- 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.
- 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.
- 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.
|Wikimedia Commons has media related to Vela Pulsar.|
- Vela Pulsar at SIMBAD
- Vela Pulsar Glitch Caught 2004/07/07
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- New Chandra Movie Features Neutron Star Action
- Sound of Vela Pulsar — recorded by Jodrell Bank Observatory