The proper motion of the VELA pulsar

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

doi:10.1086/185509

Cited by 51 publications

(31 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The components of the proper motion of the Vela pulsar with respect to the LSR become µ α cos(δ) = −37.2 ± 1.2 mas yr −1 , µ δ = 28.2 ± 1.3 mas yr −1 , for a resulting position angle of 307.2 ± 1.6 • . We note that a very similar result (µ α cos(δ) = −38.3 ± 1.2 mas yr −1 , µ δ = 27.4 ± 1.3 mas yr −1 , P.A.=305.6 ± 1.6 • ) is obtained using the correction for the Sun peculiar motion adopted by Bailes et al(1989).…”

Section: The Proper Motionsupporting

confidence: 76%

The Distance to the Vela Pulsar Gauged withHubble Space TelescopeParallax Observations

Caraveo

Luca

Mignani

et al. 2001

ApJ

121

115

View full text Add to dashboard Cite

The distance to the Vela pulsar (PSR B0833−45) has been traditionally assumed to be 500 pc. Although affected by a significant uncertainty, this value stuck to both the pulsar and the SNR. In an effort to obtain a model free distance measurement, we have applied high resolution astrometry to the pulsar V ∼ 23.6 optical counterpart. Using a set of five HST/WFPC2 observations, we have obtained the first optical measurement of the annual parallax of the Vela pulsar. The parallax turns out to be 3.4±0.7 mas, implying a distance of 294 −50 +76 pc, i.e. a value significantly lower than previously believed. This affects the estimate of the pulsar absolute luminosity and of its emission efficiency at various wavelengths and confirms the exceptionally high value of the N e towards the Vela pulsar. Finally, the complete parallax data base allows for a better measurement of the Vela pulsar proper motion (µ α cos(δ) = −37.2 ±1.2 mas yr −1 ; µ δ = 28.2 ±1.3 mas yr −1 after correcting for the peculiar motion of the Sun) which, at the parallax distance, implies a transverse velocity of ≈ 65 km sec −1 . Moreover, the proper motion position angle appears specially well aligned with the axis of symmetry of the X-ray nebula as seen by Chandra. Such an alignment allows to assess the space velocity of the Vela pulsar to be 81 km sec −1 .

show abstract

Section: The Proper Motionsupporting

confidence: 76%

The Distance to the Vela Pulsar Gauged withHubble Space TelescopeParallax Observations

Caraveo

Luca

Mignani

et al. 2001

ApJ

121

115

View full text Add to dashboard Cite

show abstract

“…2 m a s y r _ 1 and fig = 30.5 ± 0.1 m a s y r -1 , respectively. The parallax of Vela: 7rv e i a = 3.16±0.33 mas, which corresponds to a distance of £Vela = 316^29 p c The tangential velocity of the Vela pulsar is w T = 104 k m s -1 The proper motion agrees reasonably well with that of Bailes et al (1989). The distance of 316 pc is much less than early estimates of 400-600 pc found by Milne (1968), Prentice & ter Haar (1969), and Davies (1969).…”

Section: R E S U L T S And: Discussionsupporting

confidence: 54%

Astrometry of Southern Pulsars

Legge

2000

International Astronomical Union Colloquium

View full text Add to dashboard Cite

show abstract

“…In the Ðrst two mechanisms, one member of a preexisting binary must explode as a supernova in order to form the required NS or BH. During this violent event, even a small asymmetry in the explosion will impart substantial momentum to the newly formed remnant (e.g., Dewey & Cordes 1987 ;Bailes et al 1989). Even if an initially aligned system remains bound, it is unlikely that the two stellar spin axes will remain aligned with the orbital spin axis after the supernova.…”

Section: Bardeen-petterson Effect In X-ray Binariesmentioning

confidence: 99%

Bardeen‐Petterson Effect and Quasi‐periodic Oscillations in X‐Ray Binaries

Fragile

Mathews

Wilson

2001

ApJ

View full text Add to dashboard Cite

The Bardeen-Petterson e †ect around a rapidly rotating compact object causes a tilted accretion disk to warp into the equatorial plane of the rotating body. Viscous forces cause the accretion Ñow to divide into two distinct regionsÈan inner aligned accretion disk and an outer tilted accretion disk. The transition between these two occurs at a characteristic radius that depends on the mass and angular momentum of the central object and possibly on the accretion rate through the disk. We propose that accreting material passing through the transition region may generate quasi-periodic brightness oscillations such as have been observed in a number of X-ray binaries. We show that this e †ect may be present in the black hole X-ray binary GRO J1655[40. We also argue that the quasi-periodic oscillation (QPO) frequency range predicted by this model is consistent with observed QPO frequencies in both black hole and neutron star low-mass X-ray binaries.

show abstract

The proper motion of the VELA pulsar

Cited by 51 publications

References 0 publications

The Distance to the Vela Pulsar Gauged withHubble Space TelescopeParallax Observations

The Distance to the Vela Pulsar Gauged withHubble Space TelescopeParallax Observations

Astrometry of Southern Pulsars

Bardeen‐Petterson Effect and Quasi‐periodic Oscillations in X‐Ray Binaries

Contact Info

Product

Resources

About