| | |
| | |
Stat |
Members: 3667 Articles: 2'599'751 Articles rated: 2609
08 February 2025 |
|
| | | |
|
Article overview
| |
|
Pulsar microstructure and its quasi-periodicities with the S2 VLBI system at a resolution of 62.5 nanoseconds | M.V. Popov
; N. Bartel
; W.H. Cannon
; A.Yu. Novikov
; V.I. Kondratiev
; V.I. Altunin
; | Date: |
4 Jul 2001 | Journal: | Astron.Astrophys. 396 (2002) 171-187 | Subject: | astro-ph | Affiliation: | 2,3), A.Yu. Novikov , V.I. Kondratiev , V.I. Altunin ( ASC FIAN, Moscow, Russia, York University, Department of Physics and Astronomy, Toronto, Canada, Space Geodymamics Laboratory/CRESTEch, Toronto, Canada, Jet Propulsion Laboratory, Pasadena, US | Abstract: | We report on 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+-10 mcs and confirmed microstructure with characteristic timescales between 100 and 450 mcs 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 ~10 mcs, 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 7 mcs. 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. | Source: | arXiv, astro-ph/0107073 | Services: | Forum | Review | PDF | Favorites |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
|
| |
|
|
|