Arecibo Timing and Single‐Pulse Observations of Eighteen Pulsars

Lewandowski, Wojciech; Wolszczan, A.; Feiler, Grażyna; Konacki, Maciej; Sołtysiński, Tomasz

doi:10.1086/379923

Cited by 77 publications

(71 citation statements)

References 48 publications

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“…where l is the size of the radio emission region and l ≤ c × w 0.5 , where c is the speed of light and the distance to the pulsar d = 2.7 kpc (Lewandowski et al 2004), we obtain T B ≥ 2 × 10 28 K. …”

Section: Resultsmentioning

confidence: 77%

“…A pulse whose energy exceeds the energy of the average pulse (AP) by more than a factor of 100 is encountered approximately once in 3000 observed periods. Lewandowski et al (2004) show the bursting behaviour of this pulsar, which spend 70-80% of the time in a "quasi-null" state. The amplitude of the AP formed only of "burster" pulses will be about 4 times stronger that the AP obtained by folding of all observed pulses.…”

Section: Resultsmentioning

confidence: 88%

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Detection of giant pulses in pulsar PSR J1752+2359

Ershov

Kuz’min

2005

A&A

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We report the detection of Giant Pulses (GPs) in the pulsar PSR J1752+2359. About one pulse in 270 has a peak flux density more than 40 times the peak flux density of an average pulse (AP), and the strongest GP is as large as 260. The energy of the strongest GP exceeds the energy of the average pulse by a factor of 200 which is greater than in other known pulsars with GPs. PSR J1752+2359 as well as the previously detected pulsars PSR B0031-07 and PSR B1112+50, belong to the first group of pulsars found to have GPs without a strong magnetic field at the light cylinder.

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Section: Resultsmentioning

confidence: 77%

Section: Resultsmentioning

confidence: 88%

Detection of giant pulses in pulsar PSR J1752+2359

Ershov

Kuz’min

2005

A&A

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“…Proceeding from this we found that although the pulsar motion in the ecliptic longitude taken separately (cf. Hobbs et al 2005;Lewandowski et al 2004) could be 4 For φ = 0…”

Section: Discussionmentioning

confidence: 99%

Supernova remnant S 147 and its associated neutron star(s)

Gvaramadze

2006

A&A

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The supernova remnant S 147 harbors the pulsar PSR J 0538+2817 whose characteristic age is more than an order of magnitude greater than the kinematic age of the system (inferred from the angular offset of the pulsar from the geometric center of the supernova remnant and the pulsar proper motion). To reconcile this discrepancy we propose that PSR J 0538+2817 could be the stellar remnant of the first supernova explosion in a massive binary system and therefore could be as old as its characteristic age. Our proposal implies that S 147 is the diffuse remnant of the second supernova explosion (that disrupted the binary system) and that a much younger second neutron star (not necessarily manifesting itself as a radio pulsar) should be associated with S 147. We use the existing observational data on the system to suggest that the progenitor of the supernova that formed S 147 was a Wolf-Rayet star (so that the supernova explosion occurred within a wind bubble surrounded by a massive shell) and to constrain the parameters of the binary system. We also restrict the magnitude and direction of the kick velocity received by the young neutron star at birth and find that the kick vector should not strongly deviate from the orbital plane of the binary system.

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“…The gradual rise at the onset of a burst and the slow decay from a burst to the null state are modelled by exponential functions (Lewandowski et al 2004;Gajjar et al 2014 start point and the point where the function is 90 per cent or 10 per cent of the maximum for the rise and fall, respectively. Figure 9 shows the resulting histograms for 48 burst states with high S/N burst pulses.…”

Section: Pulse Energy Variationsmentioning

confidence: 99%

Investigation of nulling and subpulse drifting properties of PSR J1727−2739

Wen

Wang

Yuan

et al. 2016

A&A

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Aims. We intend to study of the nulling and subpulse drifting in PSR J1727−2739 in detail to investigate its radiation properties. Methods. The observations were carried out on 20 March, 2004 using the Parkes 64-m radio telescope with a central frequency of 1518 MHz. A total of 5568 single pulses were analysed.Results. This pulsar shows well-defined nulls with lengths lasting from 6 to 281 pulses and separated by burst phases ranging from 2 to 133 pulses. We estimate a nulling fraction of around 68%. No emission in the average pulse profile integrated over all null pulses is detected with significance above 3σ. Most transitions from nulls to bursts are within a few pulses, whereas the transitions from bursts to nulls exhibit two patterns of decay; these transitions either decrease gradually or rapidly. In the burst phase, we find that there are two distinct subpulse drift modes with vertical spacing between the drift bands of 9.7 ± 1.6 and 5.2 ± 0.9 pulse periods, while sometimes there is a third mode with no subpulse drifting. Some mode transitions occur within a single burst, while others are separated by nulls. Different modes have different average pulse profiles. Possible physical mechanisms are discussed.

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Arecibo Timing and Single‐Pulse Observations of Eighteen Pulsars

Cited by 77 publications

References 48 publications

Detection of giant pulses in pulsar PSR J1752+2359

Detection of giant pulses in pulsar PSR J1752+2359

Supernova remnant S 147 and its associated neutron star(s)

Investigation of nulling and subpulse drifting properties of PSR J1727−2739

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