The Pulse-Height Distribution for NP 0532

Argyle, Edward; Gower, J. F. R.

doi:10.1086/180991

Cited by 66 publications

(59 citation statements)

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“…Traditionally, giant-pulse amplitude distributions have been characterized as power laws (e.g. Argyle & Gower 1972;Lundgren et al 1995). The histograms shown here have roughly power-law segments to their distributions but there are outlier pulses at especially high S/N at both frequencies.…”

Section: Amplitude and Timing Statistics Of Giant Pulsesmentioning

confidence: 69%

“…Roughly, a power law with slope ≈ −2.3 can be drawn through the MP histogram at 0.43 GHz in Figure 2 and a slope ≈ −2.9 at 8.8 GHz (Figure 3. These can be compared with slopes of approximately -2.5 at 0.146 GHz (Argyle & Gower 1972) and -3.6 at 0.812 GHz (Lundgren et al 1995). Overall there thus appears to be steepening of the histogram in going from low to high frequencies.…”

Section: Amplitude and Timing Statistics Of Giant Pulsesmentioning

confidence: 90%

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The Brightest Pulses in the Universe: Multifrequency Observations of the Crab Pulsar’s Giant Pulses

Cordes

Bhat

Hankins

et al. 2004

ApJ

177

255

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We analyze the Crab pulsar at ten frequencies from 0.43 to 8.8 GHz using data obtained at the Arecibo Observatory and report the spectral dependence of all pulse components and the rate of occurrence of large-amplitude 'giant' pulses. Giant pulses occur only in the main-and-interpulse components that are manifest from radio frequencies to gamma-ray energies (known as the 'P1' and 'P2' components in the high-energy literature). Individual giant pulses reach brightness temperatures of at least 10 32 K in our data, which do not resolve the narrowest pulses, and are known to reach 10 37 K in nanosecond-resolution observations (Hankins et al. 2003). The Crab pulsar's pulses are therefore the brightest known in the observable universe. As such, they represent an important milestone for theories of the pulsar emission mechanism to explain. In addition, their short durations allow them to serve as especially sensitive probes of the Crab Nebula and the interstellar medium. We identify and quantify frequency structure in individual giant pulses using a scintillating, amplitude-modulated, polarized shot-noise model (SAMPSN). The frequency structure associated with multipath propagation decorrelates on a time scale ∼ 25 sec at 1.5 GHz. To produce this time scale requires multipath propagation to be strongly influenced by material within the Crab Nebula. We also show that some frequency structure decorrelates rapidly, on time scales less than one spin period, as would be expected from the shot-noise pattern of nanosecond duration pulses emitted by the pulsar. We discuss the detectability of individual giant pulses as a function of frequency and provenance. Taking into account the Crab pulsar's locality inside a bright supernova remnant, we conclude that the brightest pulse in a typical 1-hour observation would be most easily detectable in our lowest frequency band (0.43 GHz) to a distance ∼ 1.6 Mpc at 5σ. We also discuss the detection of such pulses using future instruments such as LOFAR and the SKA.

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Section: Amplitude and Timing Statistics Of Giant Pulsesmentioning

confidence: 69%

Section: Amplitude and Timing Statistics Of Giant Pulsesmentioning

confidence: 90%

The Brightest Pulses in the Universe: Multifrequency Observations of the Crab Pulsar’s Giant Pulses

Cordes

Bhat

Hankins

et al. 2004

ApJ

177

255

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“…(3)), which is comparable to the top end of the luminosity distribution in our own galaxy. Any M 31 pulsars that emit giant pulses (Argyle & Gower 1972) could be discovered more easily through these giant pulses than through their periodicity if the flux ratio between giant and normal pulses exceeds 10 5 (McLaughlin & Cordes 2003). Two young pulsars, the Crab pulsar B0531+21 and LMC pulsar B0540-69 (Staelin & Reifenstein 1968;Johnston & Romani 2003), are known to emit such giant pulses and the former was indeed discovered through them.…”

Section: Pulsars In Other Galaxiesmentioning

confidence: 99%

Finding pulsars with LOFAR

Leeuwen¹,

Stappers

2010

A&A

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We investigate the number and type of pulsars that will be discovered with the low-frequency radio telescope LOFAR. We consider different search strategies for the Galaxy, for globular clusters and for other galaxies. We show that a 25-day all-sky Galactic survey can find approximately 900 new pulsars, probing the local pulsar population to a deep luminosity limit. For targets of smaller angular size such as globular clusters and galaxies many LOFAR stations can be combined coherently, to make use of the full sensitivity. Searches of nearby northern-sky globular clusters can find new low luminosity millisecond pulsars. Giant pulses from Crab-like extragalactic pulsars can be detected out to over a Mpc.

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“…Argyle & Gower 1972), while that of "normal" pulses follows a log-normal distribution (Burke-Spolaor et al…”

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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The Pulse-Height Distribution for NP 0532

Cited by 66 publications

References 0 publications

The Brightest Pulses in the Universe: Multifrequency Observations of the Crab Pulsar’s Giant Pulses

The Brightest Pulses in the Universe: Multifrequency Observations of the Crab Pulsar’s Giant Pulses

Finding pulsars with LOFAR

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

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