Improved parameters for 67 pulsars from timing observations

Backus, P. R.; Taylor, J. H.; Damashek, M.

doi:10.1086/183770

Cited by 46 publications

(25 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Presumably it is one of a class of objects that represent the missing link between canonical and millisecond pulsars. If so, it confirms a long-standing conjecture that millisecond pulsars are formed by accretion onto canonical pulsars ( [2,3,18]). Many other accreting X-ray sources have been discovered consisting of a neutron star and a low-mass companion from which material is gathered, presumably, from an accretion disk ( [21,20,22,23]).…”

Section: Motivationsupporting

confidence: 78%

Lower Limit on Radius as a Function of Mass for Neutron Stars

Glendenning

2000

Phys. Rev. Lett.

View full text Add to dashboard Cite

Section: Motivationsupporting

confidence: 78%

Lower Limit on Radius as a Function of Mass for Neutron Stars

Glendenning

2000

Phys. Rev. Lett.

View full text Add to dashboard Cite

“… References: (1) Shabanova (1990); (2) Lyne (1987); (3) Downs (1982); (4) Lohsen (1981); (5) Lyne, Pritchard & Graham‐Smith (1993); (6) Lyne & Pritchard (1989); (7) Gullahorn & Rankin (1978); (8) Gullahorn & Rankin (1982); (9) D'Alessandro et al (1993); (10) Urama & Flanagan (in preparation); (11) Newton, Manchester & Cooke (1981); (12) Cordes et al (1988), and references therein; (13) Flanagan (1995), and references therein; (14) Flanagan (1996); (15) D'Alessandro & McCulloch (1997); (16) Kaspi et al (1992); (17) Johnston et al (1995); (18) Manchester et al (1978); (19) Flanagan (1993); (20) Shemar & Lyne (1996); (21) McKenna & Lyne (1990); (22) Lyne et al (1996); (23) Kaspi et al (1993); (24) Shabanova (1998); (25) Backus, Taylor & Damashek (1982). …”

Section: Glitch Size Distributionmentioning

confidence: 99%

Vela-size glitch rates in youthful pulsars

Urama

Okeke

1999

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

A total of 71 glitches (Δνν≥10‐9) have been reported to date in 30 pulsars. 13 of these glitches come from the Vela pulsar, whose glitches are mostly of magnitude Δνν∼10‐6. Only about 40 per cent of the total glitches are of this magnitude. While glitches of this size have been observed from pulsars aged 104–107 yr, 80 per cent of them come from the youthful pulsars, aged 104–105 yr. For pulsars older than 104 yr, the glitch activity is found to be proportional to the logarithm of the spin‐down rate, ν˙. Based on this relationship, we identify six other pulsars that are most likely to yield frequent large glitches. Since these pulsars are of comparable ages to the Vela pulsar, real‐time glitch detection on them and studies of their subsequent recovery would play a vital role in improving understanding of the neutron star interior and the pulsar glitch mechanisms.

show abstract

“…To combat such effects, two surveys have been conducted at low latitude and high radio frequency, with 40 pulsars found at Jodrell Bank (Clifton & Lyne 1986, Clifton et al 1992) and 45 at Parkes (Johnston et al 1992a, Johnston et al 1992b. These new samples have a mean characteristic age of less than 76 Lyne Shemar & Lyne(1996) V:McKenna h Lyne(1990) W:Lyne et al(1996) X: Kaspi et al(1993) Y: Gullahorn et al(1976) Z: Backus et al(1982) a million years compared with 6 million years for all pulsars found in previous surveys (Clifton et al 1992). Already 20 glitches have occurred in these pulsars (Shemar & Lyne 1996).…”

Section: The Frequency Of Glitchesmentioning

confidence: 99%

Rotational Instabilities in Pulsars

Lyne

1996

International Astronomical Union Colloquium

View full text Add to dashboard Cite

Abstract. In general, radio pulsars are superb clocks. However a few years after their discovery, it became clear that some pulsars show significant departures from their regular slow-down which make their rotation unpredictable. Two main forms of irregularities have been identifiedglitches and timing noise -which are most marked in, but not confined to, young pulsars. Both are probably related to the internal structure of the neutron star and the properties of the internal neutron superfluid which prevent the smooth outward flow of angular momentum as the star slows down. In this review, the observational status and statistical aspects of the phenomena are described. We do not discuss in any detail their implications for neutron star structure. Rather, we consider them in so far as they limit studies in which the rotational stability is paramount and may limit the use of pulsars as astronomical chronometers. Glitch activity, the amount of post-glitch relaxation and the amplitude of timing noise all depend roughly linearly on the frequency derivative, implying that even the millisecond pulsars are prone to these effects.

show abstract

Improved parameters for 67 pulsars from timing observations

Cited by 46 publications

References 0 publications

Lower Limit on Radius as a Function of Mass for Neutron Stars

Lower Limit on Radius as a Function of Mass for Neutron Stars

Vela-size glitch rates in youthful pulsars

Rotational Instabilities in Pulsars

Contact Info

Product

Resources

About