Pulsar Radio Emission by Conversion of Plasma Wave Turbulence: Nanosecond Time Structure

Weatherall, James C.

doi:10.1086/306218

Cited by 67 publications

(100 citation statements)

References 22 publications

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“…τ e ∼ 10 −10 s, very similar to the nano pulses proposed i.e. by Weatherall (1998) and also evident in the PIC-simulations of Jaroschek & Lesch (2006). The decay of the electric potential of a nano-pulse may be described by Φ(t) = Φ 0 · e −t/τ e with (t > 0).…”

Section: The Shape Of Pulsar Spectrasupporting

confidence: 84%

Observations of pulsars at 9 millimetres

Löhmer

Jessner

Krämer

et al. 2008

A&A

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Aims. The behaviour of the pulsar spectrum at high radio frequencies can provide decisive information about the nature of the radio emission mechanism. Methods. We report recent observations of a selected sample of pulsars at λ = 9 mm (32 GHz) with the 100-m Effelsberg radio telescope. Results. Three pulsars, PSR B0144+59, PSR B0823+26, and PSR B2022+50, were detected for the first time at this frequency. We confirm the earlier flux density measurements for a sample of six pulsars, and we are able to place upper flux density limits for another 12 pulsars. We find that all pulsar spectra have a simple form that can be described using only three parameters, one of which is the lifetime of short nano-pulses in the emission region. The study of the transition region from coherent to incoherent emission needs further and more sensitive observations at even higher radio frequencies.

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Section: The Shape Of Pulsar Spectrasupporting

confidence: 84%

Observations of pulsars at 9 millimetres

Löhmer

Jessner

Krämer

et al. 2008

A&A

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“…Observations by Hankins et al (2003) revealed that giant pulses at 5.5 GHz contain nanosecond wide subpulses and the presence of such narrow features has been predicted in numerical modelling by Weatherall (1998). At these frequencies the radio emission character of the Crab pulsar changes, with the interpulse emission becoming dominant.…”

Section: Introductionmentioning

confidence: 82%

Giant pulses from the Crab pulsar

Karuppusamy

Stappers

Straten³

2010

A&A

106

111

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The Crab pulsar is well-known for its anomalous giant radio pulse emission. Past studies have concentrated only on the very bright pulses or were insensitive to the faint end of the giant pulse luminosity distribution. With our new instrumentation offering a large bandwidth and high time resolution combined with the narrow radio beam of the Westerbork Synthesis Radio Telescope (WSRT), we seek to probe the weak giant pulse emission regime. The WSRT was used in a phased array mode, resolving a large fraction of the Crab nebula. The resulting pulsar signal was recorded using the PuMa II pulsar backend and then coherently dedispersed and searched for giant pulse emission. After careful flux calibration, the data were analysed to study the giant pulse properties. The analysis includes the distributions of the measured pulse widths, intensities, energies, and scattering times. The weak giant pulses are shown to form a separate part of the intensity distribution. The large number of giant pulses detected were used to analyse scattering and scintillation in giant pulses. We report for the first time the detection of giant pulse emission at both the main-and interpulse phases within a single rotation period. The rate of detection is consistent with the appearance of pulses at either pulse phase as being independent. These pulse pairs were used to examine the scintillation timescales within a single pulse period.

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“…The physical conditions there can be much different from the regions where radio emission is placed traditionally (i.e., at low altitudes and within a small range of heights dictated by radius-to-frequency mapping). This should be taken into account by the theories of GRP generation, for example, the ones that rely on plasma turbulence (Weatherall 1998) or on the interaction between the low-and high-frequency radio beams (Petrova 2006).…”

Section: Giant Pulsesmentioning

confidence: 99%

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

Bilous

Pennucci

Demorest

et al. 2015

ApJ

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We present the results of a wideband (720-2400 MHz) study of PSR B1821-24A (J1824-2452A, M28A), an energetic millisecond pulsar (MSP) visible in radio, X-rays and γ-rays. In radio, the pulsar has a complex average profile that spans 85% of the spin period and exhibits strong evolution with observing frequency. For the first time we measure phase-resolved polarization properties and spectral indices of radio emission throughout almost all of the on-pulse window. We synthesize our findings with high-energy information to compare M28A to other known γ-ray MSPs and to speculate that M28A's radio emission originates in multiple regions within its magnetosphere (i.e., both in the slot or outer gaps near the light cylinder and at lower altitudes above the polar cap). M28A is one of a handful of pulsars that are known to emit giant radio pulses (GRPs)-short, bright radio pulses of unknown nature. We report a drop in the linear polarization of the average profile in both windows of GRP generation and also a "W"-shaped absorption feature (resembling a double notch), partly overlapping with one of the GRP windows. The GRPs themselves have broadband spectra consisting of multiple patches with Δν/ν ∼ 0.07. Although our time resolution was not sufficient to resolve the GRP structure on the μs scale, we argue that GRPs from this pulsar most closely resemble the GRPs from the main pulse of the Crab pulsar, which consist of a series of narrowband nanoshots.

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Pulsar Radio Emission by Conversion of Plasma Wave Turbulence: Nanosecond Time Structure

Cited by 67 publications

References 22 publications

Observations of pulsars at 9 millimetres

Observations of pulsars at 9 millimetres

Giant pulses from the Crab pulsar

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

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