Matter in superstrong magnetic fields and the structure of a neutron star's surface

Hillebrandt, W.; Mueller, E.

doi:10.1086/154525

Cited by 13 publications

(3 citation statements)

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“…The basic explanation for the subpulse drifting phenomenon was given by Ruderman & Sutherland (1975). Although their fundamental assumption, regarding the ion work functions, is no longer accepted (Michel 1974; Hillebrandt & Muller 1976; Fawley, Arons & Scharlemann 1977), later modifications (Cheng & Ruderman 1977a,b, 1980) have retained the explanation for drifting. Cheng & Ruderman (1977b) invoke hotspots on the polar cap to explain the cessation of drifts during nulls.…”

Section: Discussionmentioning

confidence: 99%

A study of subpulse phase correlation across nulls in PSR B0031−07

Joshi¹,

Vivekanand²

2000

Monthly Notices of the Royal Astronomical Society

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The correlation of subpulse phases across nulls is investigated in the radio pulsar PSR B0031−07, using 29 849 periods of high‐quality data obtained with the Ooty Radio Telescope (ORT) which operates at 327 MHz. Assuming that the turn‐off and turn‐on subpulse phases (the phase of the subpulse in the last period before the null and that in the first period after the null, respectively) are independent random variables, the expected distribution of their difference (i.e. the total drift) is inconsistent with the observed distribution for null transitions within the same drift mode; this implies a correlation of subpulse phase across nulls. However, this correlation decreases with null duration for both the dominant drift modes. Substantial drifting occurs during short nulls (one to four periods); the drift rate during the short nulls appears to be constant for a class A transition, whereas it decreases with null duration for class B transitions. These results, together with the reported behaviour of PSR B1944+17 and PSR B0809+74, seem to imply different time‐scales for phase correlation in different pulsars.

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Section: Discussionmentioning

confidence: 99%

A study of subpulse phase correlation across nulls in PSR B0031−07

Joshi¹,

Vivekanand²

2000

Monthly Notices of the Royal Astronomical Society

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“…In the stationary models, the inertial potential drop is not large enough to explain the entire population of observed pulsars. The gap models seem to account more naturally for characteristics of pulsar radio emission, but they face fundamental problems, principally the binding energy associated with gap formation itself (Hillebrands & Muller 1976 ;Flower et al 1977 ;Kossl et al 1988). Recently, the common conclusion that electron-positron pairs with high densities exist close to the neutron star has been questioned by several authors.…”

Section: Introductionmentioning

confidence: 99%

The Statistics of Radio Pulsars: A Spark Model

Fan

Cheng

Manchester

2001

ApJ

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We use Monte Carlo techniques to relate a theoretical pulsar emission model to the observed distributions of pulse period, magnetic Ðeld strength, distance, and luminosity of radio pulsars. We assume that the radio luminosity of pulsars is proportional to the gap potential and current Ñow from the polar cap. The current is assumed to be nonuniform and clustered in sparks, but only those sparks swept by the line of sight contribute to the observed radio luminosity. We test our model by using the Ruderman-Sutherland vacuum gap potential and Ðnd that the simulated distributions are consistent with those observed, with the exception of the period distribution. The model predicts more long-period pulsars than are observed. This discrepancy may result from the model itself, a reduced sensitivity of surveys to long-period pulsars, or the nondipole spin-down of pulsars.

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“…This process cascades into a spark of e + -e − pair plasma, which eventually produces the observed coherent microwave radio radiation. However the model requires a high work function of iron ions on the surface of the neutron star, which was later calculated to be too low (Hillebrandt & Mueller 1976;Flowers et al 1977). Cheng & Ruderman (1980, and references therein) salvaged the model by invoking e + -e − pair production by thermal X-ray photons, emitted by the hot neutron star surface, in the Coulomb field of relativistic iron ions that are no longer bound to the neutron star surface.…”

Section: Introductionmentioning

confidence: 99%

RXTE observations of single pulses of PSR B0531+21

Vivekanand

2001

A&A

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Abstract. This article is the second in a series that analyzes about 1.87 million periods of the Crab pulsar, observed by the PCA detector aboard the RXTE X-ray observatory. At these energies, the pulsar displays none of the three phenomena that are often seen in normal radio pulsars -"pulse nulling", "systematic sub-pulse drifting" and "mode changing". The presence or absence of these three behaviors in the Crab pulsar at radio wavelengths, something that has not yet been rigorously established, might be important for a satisfactory understanding of the above three phenomena.

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Matter in superstrong magnetic fields and the structure of a neutron star's surface

Cited by 13 publications

References 0 publications

A study of subpulse phase correlation across nulls in PSR B0031−07

A study of subpulse phase correlation across nulls in PSR B0031−07

The Statistics of Radio Pulsars: A Spark Model

RXTE observations of single pulses of PSR B0531+21

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