Giant pulses from the pulsar PSR B0950+08

Smirnova, T. V.

doi:10.1134/s106377291205006x

Cited by 27 publications

(32 citation statements)

References 19 publications

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“…It worth to note that distribution of GRPs in our work ( Fig. 8 (d)) differs significantly from the two-component distribution found in (Smirnova 2012) that can be explained instability of distribution on relative short duration of time.…”

Section: B0950+08 (J0953+0755)contrasting

confidence: 79%

“…Notable thirdparty peaks are interference. At the same time the strongest pulse detected during our observational program has peak flu density 16.8 kJy that is the strongest value ever detected for this pulsar (pulse as strong as 15.2 kJy was detected earlier in (Smirnova 2012)). It worth to note that distribution of GRPs in our work ( Fig.…”

Section: B0950+08 (J0953+0755)supporting

confidence: 61%

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Search for giant pulses of radio pulsars at frequency 111 MHz with LPA radio telescope

Kazantsev

Потапов

2018

Res. Astron. Astrophys.

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We have used the unique low frequency sensitivity of the Large Phased Array radio telescope of Pushchino Radio Astronomy Observatory to collect dataset of the single pulse observations of second period pulsars of the Northern hemisphere. During observational sessions of 2011 -2017 yrs. We have collected data on 71 pulsars at 111 MHz frequency using digital pulsar receiver. We have discovered Giant Radio Pulses (GRP) from pulsars B0301+09 and B1237+25, and confirmed early reported generation of anomalously strong (probable giant) pulses from B1133+16 on statistically significant dataset. Data for these pulsars and from B0950+08, B1112+50, early reported as pulsars generating GRPs were analyzed to evaluate their behavior on long time intervals. It was found that statistical criterion (power-law spectrum of GRPs distribution on energy and peak flux density) seems not to be strict for pulsars with the low magnetic field on light cylinder. Moreover, spectra of some of these pulsars demonstrate unstable behavior with the time and have complex multicomponent shape. In the dataset of B0950+08 we have detected strongest GRP from pulsars with the low magnetic field on light cylinder ever reported having the peak flux density as strong as 16.8 kJy.

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Section: B0950+08 (J0953+0755)contrasting

confidence: 79%

Section: B0950+08 (J0953+0755)supporting

confidence: 61%

Search for giant pulses of radio pulsars at frequency 111 MHz with LPA radio telescope

Kazantsev

Потапов

2018

Res. Astron. Astrophys.

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“…Our pulse with largest SNR/SNR mean pulse = 28.2 has a flux density of 42.3 ± 21 Jy. Figure 11 shows flux densities for normal pulses from PSR B0950+08 at frequencies of 408 MHz and above, along with observations of the mean and giant pulses by Singal & Vats (2012) at 103 MHz and Smirnova (2012) at 112 MHz. In addition, we have added data points for the mean and giant pulses we observed.…”

Section: Flux Densitiesmentioning

confidence: 99%

“…Their observations also suggested that the GP distribution is not uniform, with extremely active and silent days. Singal & Vats (2012) defined GPs in their observed data as pulses with flux densities at least 10 times as large at the mean pulse flux density, while Smirnova (2012) uses a factor of 5 as the threshold for GPs. We will adopt 10 times the mean pulse strength as the threshold for GPs in our data.…”

Section: Introductionmentioning

confidence: 99%

“…Although giant pulses (GPs) have been widely detected and discussed in the literature (Cognard et al 1996;Romani & Johnston 2001;Johnston & Romani 2003;Nicastro et al 2004), the mechanism for GP production remains unclear. Petrova (2004) suggests that GPs are created by induced scattering of pulsar emissions by particles of ultra-relativistic plasma in the magnetic field, possibly explaining the observations of Smirnova (2012). Other proposed mechanisms aim to explain the observed power-law statistics through wave collapse (Robinson 1996), though concerns have been raised about the potential of the wave collapse model (Cairns 2004).…”

Section: Introductionmentioning

confidence: 99%

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Observations of Giant Pulses From Pulsar B0950+08 Using Lwa1

Tsai

Simonetti

Akukwe

et al. 2015

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We report the detection of giant pulse emission from PSR B0950+08 in 24 hours of observations made at 39.4 MHz, with a bandwidth of 16 MHz, using the first station of the Long Wavelength Array, LWA1. We detected 119 giant pulses from PSR B0950+08 (at its dispersion measure), which we define as having SNRs at least 10 times larger than for the mean pulse in our data set. These 119 pulses are 0.035% of the total number of pulse periods in the 24 hours of observations. The rate of giant pulses is about 5.0 per hour. The cumulative distribution of pulse strength S is a steep power law, N (> S) ∝ S −4.7 , but much less steep than would be expected if we were observing the tail of a Gaussian distribution of normal pulses. We detected no other transient pulses in a dispersion measure range from 1 to 90 pc cm −3 , in the beam tracking PSR B0950+08. The giant pulses have a narrower temporal width than the mean pulse (17.8 ms, on average, vs. 30.5 ms). The pulse widths are consistent with a previously observed weak dependence on observing frequency, which may be indicative of a deviation from a Kolmogorov spectrum of electron density irregularities along the line of sight. The rate and strength of these giant pulses is less than has been observed at ∼100 MHz. Additionally, the mean (normal) pulse flux density we observed is less than at ∼100 MHz. These results suggest this pulsar is weaker and produces less frequent giant pulses at 39 MHz than at 100 MHz.for gravitational-wave events, triggered by the detection of radio transients. The benefits of such collaborative work will be described in another publication.We would like to acknowledge insightful discussions with S.W. Ellingson, T.J.W. Lazio and P. S. Ray.

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Pulsar giant pulse: Coherent instability near light cylinder

Wang

Zhang

et al. 2019

Sci. China Phys. Mech. Astron.

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Giant pulses (GPs) are extremely bright individual pulses of radio pulsar. In microbursts of Crab pulsar, which is an active GP emitter, zebra-pattern-like spectral structures are observed, which are reminiscent of the "zebra bands" that are observed in type IV solar radio flares. However, band spacing linearly increases with the band center frequency of ∼ 5 − 30 GHz. In this study, we propose that the Crab pulsar GP can originate from the coherent instability of plasma near a light cylinder. Further, the growth of coherent instability can be attributed to the resonance observed between the cyclotron-resonant-excited wave and the background plasma oscillation. The particles can be injected into the closed-field line regions owing to magnetic reconnection near a light cylinder. These particles introduce a large amount of free energy that further causes cyclotron-resonant instability, which grows and amplifies radiative waves at frequencies close to the electron cyclotron harmonics that exhibit zebra-pattern-like spectral band structures. Further, these structures can be modulated by the resonance between the cyclotron-resonant-excited wave and the background plasma oscillation. In this scenario, the band structures of the Crab pulsar can be well fitted by a coherent instability model, where the plasma density of a light cylinder should be ∼ 10 13−15 cm −3 , with an estimated gradient of > 5.5 × 10 5 cm −4 . This process may be accompanied by high-energy emissions. Similar phenomena are expected to be detected in other types of GP sources that have magnetic fields of ≃ 10 6 G in a light cylinder.

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Giant pulses from the pulsar PSR B0950+08

Cited by 27 publications

References 19 publications

Search for giant pulses of radio pulsars at frequency 111 MHz with LPA radio telescope

Search for giant pulses of radio pulsars at frequency 111 MHz with LPA radio telescope

Observations of Giant Pulses From Pulsar B0950+08 Using Lwa1

Pulsar giant pulse: Coherent instability near light cylinder

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