C.D.S. - SIMBAD4 rel 1.7 - 2020.08.09CEST05:22:43

2002A&A...396..171P - Astronomy and Astrophysics, volume 396, 171-187 (2002/12-2)

Pulsar microstructure and its quasi-periodicities with the S2 VLBI system at a resolution of 62.5 nanoseconds.


Abstract (from CDS):

We report a study of microstructure and its quasi-periodicities of three pulsars at 1.65 GHz with the S2 VLBI system at a resolution of 62.5 ns, by far the highest for any such statistical study yet. For PSR B1929+10 we found in the average cross-correlation function (CCF) broad microstructure with a characteristic timescale of 95±10µs and confirmed microstructure with characteristic timescales between 100 and 450µs for PSRs B0950+08 and B1133+16. On a finer scale PSRs B0950+08, B1133+16 (component II) and B1929+10 show narrow microstructure with a characteristic timescale in the CCFs of ∼10µs, the shortest found in the average CCF or autocorrelation function (ACF) for any pulsar, apart perhaps for the Crab pulsar. Histograms of microstructure widths are skewed heavily toward shorter timescales but display a sharp cutoff. The shortest micropulses have widths between 2 and 7µs. There is some indication that the timescales of the broad, narrow, and shortest micropulses are, at least partly, related to the widths of the components of the integrated profiles and the subpulse widths. If the shortest micropulses observed are indeed due to beaming then the ratio, γ, of the relativistic energy of the emitting particles to the rest energy is about 20000, independent of the pulsar period. We predict an observable lower limit for the width of micropulses from these pulsars at 1.65 GHz of 0.5µs. If the short micropulses are instead interpreted as a radial modulation of the radiation pattern, then the associated emitting sources have dimensions of about 3km in the observer's frame. For PSRs B0950+08 and B1133+16 (both components) the micropulses had a residual dispersion delay over a 16-MHz frequency difference of ∼2µs when compared to that of average pulse profiles over a much larger relative and absolute frequency range. This residual delay is likely the result of propagation effects in the pulsar magnetosphere that contribute to limiting the width of micropulses. No nanopulses or unresolved pulse spikes were detected. Cross-power spectra of single pulses show a large range of complexity with single spectral features representing classic quasi-periodicities and broad and overlapping features with essentially no periodicities at all. Significant differences were found for the two components of PSR B1133+16 in every aspect of our statistical analysis of micropulses and their quasi-periodicities. Asymmetries in the magnetosphere and the hollow cone of emission above the polar cap of the neutron star may be responsible for these differences.

Abstract Copyright:

Journal keyword(s): stars: pulsars: general - radio continuum: stars - methods: data analysis - methods: observational

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
1 PSR J0437-47 Psr 04 37 15.7976203608 -47 15 08.536908257           DC 755 0
2 PSR B0809+74 Psr 08 14 59.500 +74 29 05.70           ~ 365 0
3 PSR B0950+08 Psr 09 53 09.3 +07 55 36           ~ 693 2
4 PSR B1133+16 Psr 11 36 03.180 +15 51 09.62           ~ 610 0
5 PSR B1929+10 Psr 19 32 13.79 +10 59 33.2           ~ 696 0
6 PSR B2016+28 Psr 20 18 03.9004752640 +28 39 54.932845661           ~ 331 0

    Equat.    Gal    SGal    Ecl

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