Monitoring of the radio emission of the Crab Nebula pulsar at low frequencies

Kuz’min, A. D.; Belyatsky, Yu. A.; Dumsky, D. V.; Izvekova, V. A.; Lapaev, K. A.; Логвиненко, С. В.; Losovsky, B. Ya.; Pugachev, V. D.

doi:10.1134/s1063772911040032

Cited by 8 publications

(4 citation statements)

References 14 publications

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“…At 330 MHz the MP and IP are much wider due to large DM smearing, which at the top of the band (440 MHz) is 0.3 ms and at the bottom (220 MHz) is 2.4 ms. The scattering time, estimated from Kuz'min et al (2011), is 470 µs at the top of the band and 5.8 ms at the bottom, and the sampling time is 819.2 µs. This leads to an effective resolution of 990 µs at the top of the band and 6.3 ms at the bottom.…”

Section: Discussionmentioning

confidence: 99%

“…TABLE 2 Sampling times, DM smearing times, scattering times, and effective resolution at the top and bottom of the band for the GB43 330 MHz and 1.2 GHz observations, as well as for the GBT 350 MHz observation. The DM smearing times were calculated using the delay between two consecutive channels caused by dispersion, and the scattering times were estimated from Kuz'min et al (2011). The sampling time listed for the 1.2 GHz GB43 observation was the most common sampling time from Table 1.…”

Section: Tablementioning

confidence: 99%

“…Notes. The DM smearing times were calculated using the delay between two consecutive channels caused by dispersion, and the scattering times were estimated from Kuz'min et al (2011). The sampling time listed for the 1.2 GHz GB43 observation was the most common sampling time from Table 1. width at low frequency is due largely to DM smearing, which is on the order of 2.4 ms at the bottom of the band.…”

Section: Radio Observationsmentioning

confidence: 99%

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A Giant Sample of Giant Pulses From the Crab Pulsar

Mickaliger

McLaughlin

Lorimer

et al. 2012

ApJ

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We observed the Crab pulsar with the 43 m telescope in Green Bank, WV over a timespan of 15 months. In total we obtained 100 hr of data at 1.2 GHz and seven hours at 330 MHz, resulting in a sample of about 95,000 giant pulses (GPs). This is the largest sample, to date, of GPs from the Crab pulsar taken with the same telescope and backend and analyzed as one data set. We calculated power-law fits to amplitude distributions for main pulse (MP) and interpulse (IP) GPs, resulting in indices in the range of 2.1-3.1 for MP GPs at 1.2 GHz and in the range of 2.5-3.0 and 2.4-3.1 for MP and IP GPs at 330 MHz. We also correlated the GPs at 1.2 GHz with GPs from the Robert C. Byrd Green Bank Telescope (GBT), which were obtained simultaneously at a higher frequency (8.9 GHz) over a span of 26 hr. In total, 7933 GPs from the 43 m telescope at 1.2 GHz and 39,900 GPs from the GBT were recorded during these contemporaneous observations. At 1.2 GHz, 236 (3%) MP GPs and 23 (5%) IP GPs were detected at 8.9 GHz, both with zero chance probability. Another 15 (4%) low-frequency IP GPs were detected within one spin period of high-frequency IP GPs, with a chance probability of 9%. This indicates that the emission processes at high and low radio frequencies are related, despite significant pulse profile shape differences. The 43 m GPs were also correlated with Fermi γ -ray photons to see if increased pair production in the magnetosphere is the mechanism responsible for GP emission. A total of 92,022 GPs and 393 γ -ray photons were used in this correlation analysis. No significant correlations were found between GPs and γ -ray photons. This indicates that increased pair production in the magnetosphere is likely not the dominant cause of GPs. Possible methods of GP production may be increased coherence of synchrotron emission or changes in beaming direction.

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Section: Discussionmentioning

confidence: 99%

Section: Tablementioning

confidence: 99%

Section: Radio Observationsmentioning

confidence: 99%

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A Giant Sample of Giant Pulses From the Crab Pulsar

Mickaliger

McLaughlin

Lorimer

et al. 2012

ApJ

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“…The resulting values β are listed in the Table 1. Some other authors (for example, Kuz'min & Dagkesamanskaya, 1983;Kuz'min et al, 1984;Lyne & Manchester, 1988) carried out calculations of the angle β earlier for the shorter samples of pulsars using some additional assumptions.…”

Section: Using Position Angles and Shapes Of Average Profilesmentioning

confidence: 99%

On magnetic fields of radio pulsars

Nikitina,

Malov

2016

Preprint

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We used the magneto-dipole radiation mechanism for the braking of radio pulsars to calculate the new values of magnetic inductions at the surfaces of neutron stars. For this aim we estimated the angles β between the rotation axis and the magnetic moment of the neutron star for 376 radio pulsars using three different methods. It was shown that there was the predominance of small inclinations of the magnetic axes. Using the obtained values of the angle β we calculated the equatorial magnetic inductions for pulsars considered. These inductions are several times higher as a rule than corresponding values in the known catalogs.keywords magnetic fields; methods: data analysis; methods: statistical; (stars:) pulsars: general

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