We present and analyse a catalogue of 233 pulsars with proper motion measurements. The sample contains a wide variety of pulsars including recycled objects and those associated with globular clusters or supernova remnants. After taking the most precise proper motions for those pulsars for which multiple measurements are available, the majority of the proper motions (58 per cent) are derived from pulsar timing methods, 41 per cent using interferometers and the remaining 1 per cent using optical telescopes. Many of the one-dimensional (1D) and two-dimensional (2D) speeds (referring to speeds measured in one coordinate only and the magnitudes of the transverse velocities, respectively) derived from these measurements are somewhat lower than earlier estimates because of the use of the most recent electron density model in determining pulsar distances. The mean 1D speeds for the normal and recycled pulsars are 152(10) and 54(6) km s −1 , respectively. The corresponding mean 2D speeds are 246(22) and 87(13) km s −1 . PSRs B2011+38 and B2224+64 have the highest inferred 2D speeds of ∼1600 km s −1 .W estudy the mean speeds for different subsamples and find that, in general, they agree with previous results. Applying a novel deconvolution technique to the sample of 73 pulsars with characteristic ages less than 3 Myr, we find the mean threedimensional (3D) pulsar birth velocity to be 400(40) km s −1 . The distribution of velocities is well described by a Maxwellian distribution with 1D rms σ = 265 km s −1 . There is no evidence for a bimodal velocity distribution. The proper motions for PSRs B1830−08 and B2334+61 are consistent with their proposed associations with the supernova remnants W41 and G114.3+0.3, respectively. Ke yw ords: stars: kinematics ‐ pulsars: general.

A statistical study of 233 pulsar proper motions

Neutron Stars 1: Equation of State and Structure

This catalog summarizes 117 high-confidence > 0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data, through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions.

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The second fermi large area telescope catalog of gamma-ray pulsars

Pulsars steadily dissipate their rotational energy via relativistic winds. Confinement of these outflows generates luminous pulsar wind nebulae, seen across the electromagnetic spectrum in ...

/pdf/the-evolution-and-structure-of-pulsar-wind-nebulae-55f6bs1qps.pdf

The evolution and structure of pulsar wind nebulae

A new classification of neutron star cooling scenarios, involving either "minimal" cooling or "enhanced" cooling, is proposed. The minimal cooling scenario replaces and extends the so-called standard cooling scenario to include neutrino emission from the Cooper pair breaking and formation process. This emission dominates that due to the modified Urca process for temperatures close to the critical temperature for superfluid pairing. Minimal cooling is distinguished from enhanced cooling by the absence of neutrino emission from any direct Urca process, due either to nucleons or to exotica such as hyperons, Bose condensates, or deconfined quarks. Within the minimal cooling scenario, theoretical cooling models can be considered to be a four parameter family involving the equation of state (including various compositional possibilities) of dense matter, superfluid properties of dense matter, the composition of the neutron star envelope, and the mass of the neutron star. The consequences of minimal cooling are explored through extensive variations of these parameters. The results are compared with the inferred properties of thermally emitting neutron stars in order to ascertain if enhanced cooling occurs in any of them. All stars for which thermal emissions have been clearly detected are at least marginally consistent with the lack of enhanced cooling, given the combined uncertainties in ages and temperatures or luminosities. The two pulsars PSR 0833-45 (Vela) and PSR 1706-44 would require enhanced cooling in case their ages and/or temperatures are on the lower side of their estimated values, whereas the four stars PSR 0656+14, PSR 1055-52, Geminga, and RX J0720.4-3125 may require some source of internal heating in case their age and/or luminosity are on the upper side of their estimated values. The new upper limits on the thermal luminosity of PSR J0205+6449 (in the supernova remnant 3C 58) and RX J0007.0+7302 (in CTA 1) are indicative of the occurrence of some enhanced neutrino emission beyond the minimal scenario.

https://iopscience.iop.org/article/10.1086/424844/pdf

Minimal Cooling of Neutron Stars: A New Paradigm

The Vela pulsar is the brightest pulsar at radio wavelengths. It was the object that told us (via its glitching) that pulsars were solid rotating bodies not oscillating ones. Along with the Crab pulsar, is it the source of many of the models of pulsar behavior. Therefore it is of vital importance to know how far away it is and its origin. The proper motion and parallax for the Vela pulsar have been derived from 2.3 and 8.4 GHz very long baseline interferometry (VLBI) observations. The data span 6.8 years and consist of 11 epochs. We find a proper motion of μα cos δ = -49.68 ± 0.06, μδ = 29.9 ± 0.1 mas yr-1 and a parallax of 3.5 ± 0.2 mas, which is equivalent to a distance of 287 pc. When we subtract out the Galactic rotation and solar peculiar velocity, we find μ* = 45 ± 1.3 mas yr-1 with a position angle of 301° ± 18 which implies that the proper motion has a small but significant offset from the X-ray nebula's symmetry axis.

https://iopscience.iop.org/article/10.1086/378089/pdf

The Vela Pulsar’s Proper Motion and Parallax Derived from VLBI Observations

The Vela pulsar is the brightest pulsar at radio wavelengths. It was the object that told us (via its glitching) that pulsars were solid rotating bodies not oscillating ones. Along with the Crab pulsar is it the source of many of the models of pulsar behavior. Therefore it is of vital importance to know how far away it is, and its origin. 
The proper motion and parallax for the Vela pulsar have been derived from 2.3 and 8.4 GHz Very Long Baseline Interferometry (VLBI) observations. The data spans 6.8 years and consists of eleven epochs. We find a proper motion of $\mu_{\alpha {\rm cos}\delta}= -49.61 \pm 0.06, \mu_\delta= 29.8 \pm 0.1$ \myr and a parallax of $3.4 \pm 0.2$ mas, which is equivalent to a distance of $293_{-17}^{+19}$ pc. When we subtract out the galactic rotation and solar peculiar velocity we find $\mu_* = 45 \pm 1.3$ \myr with a position angle (PA) of $301^\circ\pm1.8$ which implies that the proper motion has a small but significant offset from the X-ray nebula's symmetry axis.

https://arxiv.org/pdf/astro-ph/0302374.pdf

The Vela Pulsar's proper motion and parallax derived from VLBI observations

Of all pulsars known, Vela has been one of the most productive in terms in understanding pulsars and their characteristics. We present the latest results derived from Australian telescopes. These include a more accurate pulsar distance, a more precise pulsar local space velocity, a new model of spin-up at a glitch, and the association of a radio nebula with the X-ray pulsar wind nebula.

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The Vela Pulsar, the Key?

Of all pulsars known Vela has been one of the most productive in terms in understanding pulsars and their characteristics. We present the latest results derived from Australian telescopes. These include a more accurate pulsar distance, a more precise pulsar local space velocity, a new model of the spin up and the association of a radio nebula with the X-ray pulsar wind nebula.

David Legge

Papers

The Vela Pulsar’s Proper Motion and Parallax Derived from VLBI Observations

The Vela Pulsar's proper motion and parallax derived from VLBI observations

The Vela Pulsar, the Key?

The Vela pulsar, the key?

The Southern Hemisphere Contribution to the VSOP Mission