A Broadband Radio Study of the Average Profile and Giant Pulses From PSR B1821-24a

Bilous, A. V.; Pennucci, T. T.; Demorest, Paul; Ransom, S. M.

doi:10.1088/0004-637x/803/2/83

Cited by 37 publications

(35 citation statements)

References 89 publications

(164 reference statements)

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“…GRPs are detected from about 10 pulsars, including some young pulsars such as the Crab pulsar (PSR B0531+21) (e.g. Majid et al 2011) and PSR B0540-69 (Johnston & Romani 2003), and some millisecond pulsars such as PSR B1937+21 (Soglasnov et al 2004) and PSR B1821-24A (Bilous et al 2015). Even some of relatively slowly rotating pulsars, such as PSR B0950+08 (e.g.…”

Section: Introductionmentioning

confidence: 99%

Wide-Band Spectra of Giant Radio Pulses From the Crab Pulsar

Mikami¹,

Asano²,

Tanaka³

et al. 2016

ApJ

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We present the results of the simultaneous observation of the giant radio pulses (GRPs) from the Crab pulsar at 0.3, 1.6, 2.2, 6.7, and 8.4 GHz with four telescopes in Japan. We obtain 3194 and 272 GRPs occurring at the main pulse and the interpulse phases, respectively. A few GRPs detected at both 0.3 and 8.4 GHz are the most wide-band samples ever reported. In the frequency range from 0.3 to 2.2 GHz, we find that about 70% or more of the GRP spectra are consistent with single power laws and the spectral indices of them are distributed from −4 to −1. We also find that a significant number of GRPs have such a hard spectral index (approximately −1) that the fluence at 0.3 GHz is below the detection limit ("dim-hard" GRPs). Stacking light curves of such dim-hard GRPs at 0.3 GHz, we detect consistent enhancement compared to the off-GRP light curve. Our samples show apparent correlations between the fluences and the spectral hardness, which indicates that more energetic GRPs tend to show softer spectra. Our comprehensive studies on the GRP spectra are useful materials to verify the GRP model of fast radio bursts in future observations.

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Section: Introductionmentioning

confidence: 99%

Wide-Band Spectra of Giant Radio Pulses From the Crab Pulsar

Mikami¹,

Asano²,

Tanaka³

et al. 2016

ApJ

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“…Bilous et al (2015) note that giant pulses in B1821−24A occur at the phase of the double notches, and a peak of a narrow component in an X-ray profile of this pulsar nearly coincides with the notches.…”

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confidence: 76%

A model for distortions of polarisation-angle curves in radio pulsars

Dyks

Serylak

Osłowski

et al. 2016

A&A

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Context. Some radio pulsar profiles (in particular those of millisecond pulsars) contain wide emission structures which cover large intervals of pulse phase. Local distortions of an average curve of polarisation angle (PA) can be identified in such profiles, and they are often found to be associated with absorption features or narrow emission components. Aims. The features may be interpreted as a convolution of a lateral profile of an emitter with a microscopic radiation pattern of a non-negligible angular extent. Methods. We study a model which assumes that such an extended microbeam of the X-mode curvature radiation is spreading the radiation polarised at a fixed position angle within an interval of pulse phase. Results. The model is capable of interpreting the strongly dissimilar polarisation of double notches in PSR B1821−24A (for which we present new polarisation data from the Nançay Radio Telescope) and PSR J0437−4715. It also explains a step-like change in PA observed at the bifurcated trailing component in the profile of J0437−4715. A generic form of the modelled PA distortion is a zigzag-shaped wiggle, which in the presence of the second polarisation mode (O mode) can be magnified or transformed into a W-or U-shaped deflection of a total net PA. Conclusions. The model's efficiency in interpreting dissimilar polarisation effects provides further credence to the stream-based (fanbeam) geometry of pulsar emission. It also suggests that the microbeam width may not always be assumed negligible in comparison with the angular scale of emissivity gradients in the emission region.

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“…Within the framework of our considerations, the radio/gamma-ray correlation in the millisecond pulsars can be explained by the fact that the two types of emission result from the same plasma flow related to the outer/slot gap. Note that an idea of direct generation of radio emission in the high-altitude gaps (e.g., Espinoza et al 2013;Bilous et al 2015) encounters a difficulty of providing the necessary coherence in the outer magnetosphere. Therefore the propagation origin of the radio components correlating with gamma-ray emission seems preferable.…”

Section: Millisecond Pulsarsmentioning

confidence: 99%

“…2013; Bilous et al. 2015) encounters the difficulty of providing the necessary coherence in the outer magnetosphere. Therefore the propagation origin of the radio components correlating with gamma-ray emission seems preferable.…”

Section: Implications For Gamma-ray Pulsarsmentioning

confidence: 99%

Physics of radio emission in gamma-ray pulsars

Petrova

2016

J. Plasma Phys.

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Propagation of radio emission in a pulsar magnetosphere is reviewed. The effects of polarization transfer, induced scattering and reprocessing to high energies are analysed with a special emphasis on the implications for the gamma-ray pulsars. The possibilities of the pulsar plasma diagnostics based on the observed radio pulse characteristics are also outlined. As an example, the plasma number density profiles obtained from the polarization data for the Vela and the gamma-ray millisecond pulsars J1446-4701, J1939+2134 and J1744-1134 are presented. The number densities derived tend to be the highest/lowest when the radio pulse leads/lags the gamma-ray peak. In the PSR J1939+2134, the plasma density profiles for the main pulse and interpulse appear to fit exactly the same curve, testifying to the origin of both radio components above the same magnetic pole and their propagation through the same plasma flow in opposite directions. The millisecond radio pulse components exhibiting flat position angle curves are suggested to result from the induced scattering of the main pulse by the same particles that generate gamma rays. This is believed to underlie the wide-sense radio/gamma-ray correlation in the millisecond pulsars. The radio quietness of young gamma-ray pulsars is attributed to resonant absorption, whereas the radio loudness to the radio beam escape through the periphery of the open field line tube.

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A Broadband Radio Study of the Average Profile and Giant Pulses From PSR B1821-24a

Cited by 37 publications

References 89 publications

Wide-Band Spectra of Giant Radio Pulses From the Crab Pulsar

Wide-Band Spectra of Giant Radio Pulses From the Crab Pulsar

A model for distortions of polarisation-angle curves in radio pulsars

Physics of radio emission in gamma-ray pulsars

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