Radio Pulsars — an Observer’S Perspective

Lorimer, D. R.

doi:10.1007/978-94-010-0548-7_1

Cited by 4 publications

References 25 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

et al. 2001

The Astrophysical Journal

View full text Add to dashboard Cite

We report on five binary pulsars discovered in the Parkes multibeam Galactic plane survey. All of the pulsars are old, with characteristic ages 1-11 Gyr, and have relatively small inferred magnetic fields, 5-90e8 G. The orbital periods range from 1.3 to 15 days. As a group these objects differ from the usual low-mass binary pulsars (LMBPs): their spin periods of 9-88 ms are relatively long; their companion masses, 0.2-1.1 Msun, are, in at least some cases, suggestive of CO or more massive white dwarfs; and some of the orbital eccentricities, 1e-5 < e < 0.002, are unexpectedly large. We argue that these observed characteristics reflect binary evolution that is significantly different from that of LMBPs. We also note that intermediate-mass binary pulsars apparently have a smaller scale-height than LMBPs.Comment: 5 pages, 4 embedded EPS figs, accepted for publication by ApJ Letter

show abstract

Changing Frequency Separation of Kilohertz Quasi‐periodic Oscillations in the Sonic‐Point Beat‐Frequency Model

Lamb

Miller

2001

ApJ

105

View full text Add to dashboard Cite

Previous work on the sonic-point beat-frequency (SPBF) model of the kilohertz quasi-periodic oscillations (QPOs) observed in the X-ray flux from neutron stars in low-mass binary systems has shown that it naturally explains many properties of these QPOs. These include the existence of just two principal QPOs in a given source, the commensurability of the frequency separation ∆ν of the two kilohertz QPOs and the spin frequency ν s inferred from burst oscillations, and the high frequencies, coherence, and amplitudes of these QPOs. Here we show that the SPBF model predicts that ∆ν is less than but close to ν s , consistent with the observed differences between ∆ν and ν s . It also explains naturally the decrease in ∆ν with increasing QPO frequency seen in some sources and the plateau in the QPO frequency-X-ray flux observed in 4U 1820−30. The model fits well the QPO frequency behavior observed in Sco X-1, 4U 1608−52, 4U 1728−34, and 4U 1820−30 (χ 2 /dof = 0.4-2.1), giving masses ranging from 1.59 to 2.0 M ⊙ and spin rates ranging from 279 to 364 Hz. In the SPBF model, the kilohertz QPOs are effects of strong-field gravity. Thus, if the model is validated, the kilohertz QPOs can be used not only to determine the properties of neutron stars but also to explore quantitatively general relativistic effects in the strong-field regime.

show abstract

Radio Pulsars — an Observer’S Perspective

Abstract: Abstract. Pulsar astronomy is currently enjoying one of the most productive phases in its history. In this review, I outline some of the basic observational aspects and summarise some of the latest results of searches for pulsars in the disk of our Galaxy and its globular cluster system.

Cited by 4 publications

References 25 publications

Pulsar Timing — Strong Gravity Clock Experiments

Pulsar Timing — Strong Gravity Clock Experiments

Discovery of Five Binary Radio Pulsars

Changing Frequency Separation of Kilohertz Quasi‐periodic Oscillations in the Sonic‐Point Beat‐Frequency Model

Contact Info

Product

Resources

About