Vela Pulsar
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The Vela Pulsar (PSR B0833-45 or PSR J0835-4510) is a radio, optical, X-ray and gamma-emitting pulsar associated with Vela Supernova Remnant, in the constellation of Vela. The association of the Vela pulsar with the Vela Supernova Remnant, made by astronomers at the University of Sydney in 1968,[1] was direct observational proof that supernovae form neutron stars.
It has a period of 89 ms (the shortest known at the time of its discovery) and the remnant from the supernova explosion is estimated to be travelling at 1,200 km/s.[1] It has the third brightest optical component of all known pulsars (magnitude 23.6)[2] which pulses twice for every single radio pulse.
[edit] References
- ^ Lyne, Andrew G.; Francis Graham-Smith (1998). Pulsar Astronomy. Cambridge University Press. ISBN 0-521-59413-8.
- ^ Mignani et al (2007-10-01). "The optical spectrum of the Vela Pulsar". Astronomy & Astrophysics.
[edit] External links
- Glitch noted http://www.hartrao.ac.za/news/040707vela/index.html
- Chandra image http://chandra.harvard.edu/photo/2000/vela/index.html
- Chandra images show pronounced jet http://chandra.harvard.edu/photo/2003/vela_pulsar/index.html
