The imaging detectors of the Einstein X-ray observatory have been used to study the Vela pulsar and its surrounding region. The authors use models of magnetized hydrogen atmospheres to fit the soft X-ray thermal spectrum of the Vela pulsar obtained by ROSAT.

Soon after the detection of its radio pulses… The derived surface temperature of the star Ts∞=0.66−0.01+0.04MK (1σ level over the entire mass and radius range of our study) is consistent with earlier results. The star of this movie is the Vela pulsar, a neutron star that was formed when a massive star collapsed. Consequently the estimated S for Vela at observation frequencies between 400 MHz and 1400 MHz will be lower than actual - while for observation frequencies outside that range the estimate will be higher than actual. A reliable measurement of its surface temperature based on modeling of the surface thermal emission is of outmost importance for comparison with models of neutron star cool.. The pattern reflects numerous motions of the spacecraft, including its orbit around Earth, the precession of its orbital plane, the manner in which the LAT nods north and south on alternate orbits, and more. Nor is there evidence for other types of variability in the pulsar's X-ray … The low temperature obtained, T e ∞ … We reanalyse the X-ray spectrum of the PSR B0833–45 (the Vela pulsar) using the data of the Chandra space observatory. By P. W. Anderson, D. Pines, M. A. Alpar and J. Shaham. The Crab Pulsar appears in optical photographs as a moderately bright (magnitude 16) star in the centre of the Crab Nebula. Other articles where Vela pulsar is discussed: pulsar: Pulsars in visible light, X-rays, and gamma rays: …such as the Crab and Vela pulsars, are losing rotational energy so precipitously that they also emit radiation of shorter wavelength. The observed complex postglitch behavior of the Vela pulsar is explained as resulting from coupling of the crust to crustal neutron superfluid, specifically that part of the superfluid in which vortex lines are pinned to crustal nuclei. Pulsar Radiometer Equation Calculator : Antenna Gain (dBi): Receiver Bandwidth (MHz): ... the Vela pulsar has a 'turn-over' point near 600 MHz and falls away below this frequency. II - Vela pulsar . INTRODUCTION The Vela pulsar is the youngest pulsar for which there is strong evidence that thermal emission from the surface of the neutron star has been detected ( Ogelman, Finley & Zimmermann 1993; Ogelman 1995). Vortex creep and the internal temperature of neutron stars. In contrast to previous works, we consider a wide range of possible masses and radii of the pulsar. Abstract . However, the preferable … … Although the pulsar is a relatively strong source of X-rays, there are not detectable pulsations at the pulsar period; the pulsed X-ray luminosity is less than approximately 10 to the 31st ergs/s in the 0.1-4.5 keV band. The distance and hydrogen column density required by the authors' fits are in good agreement with other independent estimates and can be considered as an argument for the presence of hydrogen at the surface of this pulsar. It is shown how the general … The Vela pulsar outlines a fascinating pattern in this movie showing 51 months of position and exposure data from Fermi’s Large Area Telescope (LAT). The movie renders Vela’s position in a fisheye …