The parallax and proper motion of PSRI451–68

Bailes, M.; Manchester, R. N.; Kesteven, M. J.; Norris, R. P.; Reynolds, J. E.

doi:10.1038/343240a0

Cited by 46 publications

(46 citation statements)

References 15 publications

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“…There is also evidence for a counter jet in the opposite direction. These jets have a position angle of 130¡ (measured east of north), and are aligned to within 8¡^5¡ with the pulsarÏs proper motion vector (Bailes et al 1990 ;DeLuca, Mignani, & Caraveo 2000).…”

Section: An Image Of the Vela Pulsarmentioning

confidence: 99%

See 1 more Smart Citation

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

283

305

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We present high-resolution Chandra X-ray observations of PSR B0833[45, the 89 ms pulsar associated with the Vela supernova remnant. We have acquired two observations separated by 1 month to search for changes in the pulsar and its environment following an extreme glitch in its rotation frequency. We Ðnd a well-resolved nebula with a toroidal morphology remarkably similar to that observed in the Crab Nebula, along with an axial Crab-like jet. Between the two observations, taken D3 ] 105 s and D3 ] 106 s after the glitch, the Ñux from the pulsar is found to be steady to within 0.75% ; the 3 p limit on the fractional increase in the pulsarÏs X-ray Ñux is of the inferred glitch energy. We use [10~5 this limit to constrain parameters of glitch models and neutron star structure. We do Ðnd a signiÐcant increase in the Ñux of the nebulaÏs outer arc ; if associated with the glitch, the inferred propagation velocity is similar to that seen in the brightening of the Crab Nebula wisps. We propose an explana-Z0.7c, tion for the X-ray structure of the Vela synchrotron nebula based on a model originally developed for the Crab Nebula. In this model, the bright X-ray arcs are the shocked termination of a relativistic equatorial pulsar wind that is contained within the surrounding kidney-bean shaped synchrotron nebula comprising the postshock, but still relativistic, Ñow. In a departure from the Crab model, the magnetization parameter p of the Vela pulsar wind is allowed to be of order unity ; this is consistent with the simplest MHD transport of magnetic Ðeld from the pulsar to the nebula, where B ¹ 4 ] 10~4 G. The inclination angle of the axis of the equatorial torus with respect to the line of sight is identical to that of the rotation axis of the pulsar as previously measured from the polarization of the radio pulse. The projection of the rotation axis on the sky may also be close to the direction of proper motion of the pulsar if previous radio measurements were confused by orthogonal-mode polarized components. We review e †ects that may enhance the probability of alignment between the spin axis and space velocity of a pulsar, and speculate that short-period, slowly moving pulsars are just the ones best-suited to producing synchrotron nebulae with such aligned structures. Previous interpretations of the compact Vela nebula as a bow-shock in a very weakly magnetized wind su †ered from data of inadequate spatial resolution and less plausible physical assumptions.

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Section: An Image Of the Vela Pulsarmentioning

confidence: 99%

“…The proper motion of the Vela pulsar has been measured with comparable accuracy using both radio interferometry (Bailes et al 1990) and images from HST (De Luca et al 2000). The resulting mean value yr~1 at a position angle of 302¡^4¡ is 0A .056^0A .004 within 8¡ of the axis of the nebula The (( 0 ] 180¡ \ 310¡).…”

Section: Implications Of the Proper Motionmentioning

confidence: 99%

Vela Pulsar and Its Synchrotron Nebula

Helfand

Gotthelf

Halpern

2001

ApJ

283

305

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“…Nice & Taylor 1995; Toscano et al 1999b; Wolszczan et al 2000; Freire et al 2003). The poor rotational stability observed for young pulsars 1 (referred to as timing noise) affected early measurements of proper motions using timing methods; for these, interferometers had been used to obtain the proper motions (for example, Lyne, Anderson & Salter 1982; Bailes et al 1990a; Harrison, Lyne & Anderson 1993; Fomalont et al 1997; Brisken et al 2002). In Paper I we described a new method, based on the modelling and removal of timing noise from the timing residuals of young pulsars using harmonically related sinusoids, that allowed accurate proper motions to be determined using standard timing methods.…”

Section: Introductionmentioning

confidence: 99%

A statistical study of 233 pulsar proper motions

Hobbs

Lorimer

Lyne

et al. 2005

Monthly Notices of the Royal Astronomical Society

1,360

103

1,505

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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%) are derived from pulsar timing methods, 41% using interferometers and the remaining 1% using optical telescopes. Many of the 1-D and 2-D 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 1-D speeds for the normal and recycled pulsars are 152(10) and 54(6) km/s respectively. The corresponding mean 2-D speeds are 246(22) and 87(13) km/s. PSRs B2011+38 and B2224+64 have the highest inferred 2-D speeds of ~1600 km/s. We study 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 3-D pulsar birth velocity to be 400(40) km/s. The distribution of velocities is well described by a Maxwellian distribution with 1-D rms sigma=265 km/s. 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.Comment: 20 pages, accepted by MNRA

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“…It is not coincident with the prominent star near the head of the nebula. Bailes et al (1990) determine a proper motion position angle (measured through east) of θ = 269 ± 1…”

Section: Observations and Reductionmentioning

confidence: 99%

Discovery of an optical bow-shock around pulsar B0740-28

Jones

Stappers

Gaensler

2002

A&A

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Abstract.We report the discovery of a faint Hα pulsar wind nebula (PWN) powered by the radio pulsar B0740−28. The characteristic bow-shock morphology of the PWN implies a direction of motion consistent with the previously measured velocity vector for the pulsar. The PWN has a flux density more than an order of magnitude lower than for the PWNe seen around other pulsars, but, for a distance 2 kpc, it is consistent with propagation through a medium of atomic density nH ∼ 0.25 cm −3 , and neutral fraction of 1%. The morphology of the PWN in the area close to the pulsar is distinct from that in downstream regions, as is also seen for the PWN powered by PSR B2224+65. In particular, the PWN associated with PSR B0740-28 appears to close at its rear, suggesting that the pulsar has recently passed through a transition from low density to high density ambient gas. The faintness of this source underscores that deep searches are needed to find further examples of optical pulsar nebulae.

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The parallax and proper motion of PSRI451–68

Cited by 46 publications

References 15 publications

Vela Pulsar and Its Synchrotron Nebula

Vela Pulsar and Its Synchrotron Nebula

A statistical study of 233 pulsar proper motions

Discovery of an optical bow-shock around pulsar B0740-28

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