Detection of giant pulses from the pulsar PSR B1112+50

Ershov, A. A.; Kuz’min, A. D.

doi:10.1134/1.1544530

Cited by 43 publications

(37 citation statements)

References 11 publications

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“…These pulses have a slight preference to the trailing phase of the average pulse profile, although a clear phase relationship is not evident. This is similar to the giant pulse-like emission from this pulsar reported by Ershov & Kuzmin (2003). Figure 5 shows the pulse energy distribution and the bright pulses with energies greater than 10 × E comprise the trailing part of the distribution.…”

Section: Psr B1112+50supporting

confidence: 62%

A low frequency study of PSRs B1133+16, B1112+50, and B0031−07

Karuppusamy

Stappers

Serylak

2010

A&A

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We use the low frequency (110-180 MHz) capabilities of the Westerbork Synthesis Radio Telescope (WSRT) to characterise a large collection of single pulses from three low magnetic field pulsars. Using the Pulsar Machine II (PuMa-II) to acquire and coherently dedisperse the pulsar signals, we examine whether the bright pulses observed in these pulsars are related to the classical giant pulse emission. Giant pulses are reported from PSR B1112+50 and bright pulses from the PSRs B1133+16 and B0031−07. These pulsars also exhibit large intensity modulations observed as rapid changes in the single pulse intensity. Evidence of global magnetospheric effects is provided by our detection of bright double pulses in PSRs B0031−07 and B1133+16. Using the multi-frequency observations, we accurately determine the dispersion measures (4.844 ± 0.002 for B1133+16 and 9.1750 ± 0.0001 for B1112+50), derive the radio emission height in PSR B1133+16 and report on the properties of subpulse drift modes in these pulsars. We also find that these pulsars show a much larger intensity modulation at low sky frequencies resulting in narrow and bright emissions.

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Section: Psr B1112+50supporting

confidence: 62%

A low frequency study of PSRs B1133+16, B1112+50, and B0031−07

Karuppusamy

Stappers

Serylak

2010

A&A

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“…Note that the above estimates and the suggested mechanism of giant pulses on the whole are also applicable to PSR B0540-69 and PSR B1821-24. Another two pulsars recognized as giant pulse sources, PSR B1112+50 (Ershov & Kuzmin 2003) and PSR B0031-07 (Kuzmin et al 2004), appear to be quite different from the others: they have long periods and can show series of neighbouring giant pulses -a phenomenon never seen before. Interpretation of this peculiar case is beyond the framework of the present paper.…”

Section: Beam-to-beam Scatteringmentioning

confidence: 99%

On the origin of giant pulses in radio pulsars

Petrova¹

2004

A&A

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Abstract. Induced Compton scattering of radio emission off the particles of the ultrarelativistic highly magnetized plasma of pulsar magnetosphere is considered. The scattering between the photon beams of substantially differing frequencies and orientations appears to result in photon transfer to the higher frequency. With the decreasing spectrum of pulsar radio emission, this may imply a significant amplification of the higher-frequency intensity. A detailed analysis shows that the rays of widely spaced frequencies can have different orientations, at least at certain locations in the pulsar magnetosphere. The numerical estimates confirm the possibility of an efficient beam-to-beam scattering in the pulsars known as giant pulse sources. Thus, the intensity amplification on account of induced scattering of the lower-frequency radiation is suggested to underlie the giant pulse phenomenon. A huge pulse-to-pulse scatter in the observed intensities of the giant pulse sources (over more than three orders of magnitude) testifies to significant variations of the efficiency of amplification. If this variability is attributed to the fluctuations of both the particle number density and the incident intensity and the latter are considered as the partially correlated Gaussian random quantities, one arrives at the power-law distribution of strong pulses in intensity. The formation of the giant pulse substructure, the broad-band spectral behaviour of the scattering efficiency and the link of giant pulses to the high-energy emission are discussed as well.

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“…Moreover, the line width of the excited 2p state, which is determined by its decay time, is large (99.8 MHz), making the detection of the fine-structure line a difficult observation. One astrophysical setting where the feasibility of detecting such a line has been studied is the interstellar H ii regions (see, e.g., Dennison et al 2005 and references therein ;Ershov 1987), in which the excited levels are populated by recombination.…”

Section: Introductionmentioning

confidence: 99%

Hydrogen 2p–2sTransition: Signals from the Epochs of Recombination and Reionization

Sethi

Subrahmanyan

Roshi

2007

ApJ

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We propose a method to study the epoch of reionization based on the possible observation of 2pY2s fine-structure lines from the neutral hydrogen outside the cosmological H ii regions enveloping QSOs and other ionizing sources in the reionization era. We show that for parameters typical of luminous sources observed at z ' 6:3, the strength of this signal, which is proportional to the H i fraction, has a brightness temperature '20 K for a fully neutral medium. The fine-structure line from this redshift is observable at ' 1 GHz, and we discuss prospects for the detection with several operational and future radio telescopes. We also compute the characteristics of this signal from the epoch of recombination; the peak brightness is expected to be '100 K, and this signal appears in the frequency range 5Y10 MHz. The signal from the recombination era is nearly impossible to detect owing to the extreme brightness of the Galactic emission at these frequencies.

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Detection of giant pulses from the pulsar PSR B1112+50

Cited by 43 publications

References 11 publications

A low frequency study of PSRs B1133+16, B1112+50, and B0031−07

A low frequency study of PSRs B1133+16, B1112+50, and B0031−07

On the origin of giant pulses in radio pulsars

Hydrogen 2p–2sTransition: Signals from the Epochs of Recombination and Reionization

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