Vela Pulsar

Provenance-Backed Scientific Measurements

Every measurement below preserves its unit, uncertainty interval, observational method, reference epoch, quality status, and primary catalog source. See Uncertainty & Provenance for how competing measurements are handled.

J2000 Equatorial Sky Chart & Culmination Altitude

The chart below plots Vela Pulsar (PSR B0833-45) — Neutron Star at RA 08h 35m 20.66s, Dec -45° 10′ 35.2″ within Vela, alongside peak meridian transit altitudes for 40°N and 30°S observers. Use the RA/Dec Coordinate Converter to compute exact culmination altitude for your latitude.

Astrophysical Context & Structure

Discovered in 1968 by astronomers at the University of Sydney using the Molonglo Cross Radio Telescope, the Vela Pulsar (PSR B0833-45) provided the first direct observational link between a core-collapse supernova remnant and a central spinning neutron star. Located roughly 936 light-years away in Vela, it formed approximately 11,000 years ago when a massive progenitor star exploded, blowing out the sprawling 8-degree Vela Supernova Remnant.

Spinning once every 89.33 milliseconds (11.2 times per second) within a surface dipole magnetic field of 3.4 trillion gauss, the Vela Pulsar emits pulsed radiation across the entire electromagnetic spectrum—from radio waves and V = 23.6 optical flashes to X-rays and TeV gamma rays. In GeV gamma rays monitored by the Fermi Large Area Telescope, it outshines every other persistent point source in the sky. High-resolution Chandra X-ray movies of its surrounding pulsar wind nebula reveal a double-ring torus and a relativistic polar jet that coils like a garden hose while shooting particles outward at 70 percent of the speed of light.

Every two to three years, the pulsar's steady spin-down is interrupted by a sudden rotational 'glitch' in which its spin frequency jumps upward by roughly one to three parts per million within seconds. These abrupt spin-ups occur when quantized superfluid vortices pinned inside the neutron star's inner crust unpin en masse, transferring angular momentum from the faster-spinning interior superfluid to the solid outer crust.

Practical Visual Observing Guide

• The optical pulsar is extremely faint (V = 23.6), requiring 4-meter to 8-meter professional telescopes with high-speed photometers.
• The surrounding Vela Supernova Remnant filaments (Pencil Nebula, NGC 2736) are visible in amateur telescopes under dark southern skies using O-III filters.
• Easily detected at 1.4 GHz by modest amateur and educational radio dishes due to its high radio flux density.

Catalog Cross-Identifications & Aliases

Common Aliases: PSR B0833-45 · PSR J0835-4510 · 3FGL J0835.3-4510

Related Objects, Comparisons & Guides

Scientific Sources & Dataset Provenance

• SIMBAD Astronomical Database (CDS) (2026-10 release): Wenger, M., et al. 2000, A&AS, 143, 9 (The SIMBAD astronomical database) — Centre de Données astronomiques de Strasbourg