Pulsar Sub-pulses and the Emission Process

Cole, T. W.

doi:10.1038/227788a0

Cited by 21 publications

(17 citation statements)

References 10 publications

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“…• of pulse longitude (Cole 1970;Sutton et al 1970;Vitkevich & Shitov 1970;Page 1973;Bartel et al 1981;Davies et al 1984). A key to understanding why this is so may follow simply from Davies et al's discussion: They find that the driftbands at 102 MHz are "essentially straight", whereas those at 406 and 1412 MHz become increasingly curved.…”

Section: Introductionmentioning

confidence: 99%

“…Vitkevich & Shitov (1970) and Sutton et al (1970) first exhibited the star's marvelously precise "drifting" pulse sequences (hereafter PSs) early the next year, and the latter paper introduced the now standard terminology of P 1 , P 2 and P 3 for the pulsar rotation period, the subpulse-separation interval, and the driftband-separation period, respectively. Properties of these drifting subpulses have been investigated by many authors over the past three decades (e.g., Cole 1970;Taylor & Huguenin 1971;Backer et al 1975). Its polarization properties have also been studied in detail by various investigators von Hoensbroech & Xilouris 1997;Gould & Lyne 1998).…”

Section: Introductionmentioning

confidence: 99%

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PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

Rankin¹,

Ramachandran

Suleymanova

2005

A&A

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Abstract. The longitude separation between adjacent drifting subpulses, P 2 , is roughly constant for many pulsars. It was then perplexing when pulsar B0809+74 was found to exhibit substantial variations in this measure, both with wavelength and with longitude position within the pulse window. We analyze these variations between 40 and 1400 MHz, and we show that they stem primarily from the incoherent superposition of the two orthogonal modes of polarization.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

Rankin¹,

Ramachandran

Suleymanova

2005

A&A

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“…In order to investigate this new phenomenon, numerous studies were conducted (e.g. Lovelace & Craft 1968;Taylor et al 1969;Lang 1969;Sutton et al 1970;Cole 1970). The authors performed fluctuation-spectral analysis using Fourier techniques which revealed another type of characteristic frequency at which a significant amount of power was present in the fluctuation spectra of pulsars and provided evidence of a periodic modulation of pulse intensities.…”

Section: Introductionmentioning

confidence: 99%

S2DFS: analysis of temporal changes of drifting subpulses

Serylak

Stappers²,

Weltevrede³

2009

A&A

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Context. We introduce a new technique, called the sliding two-dimensional fluctuation spectrum, used for detecting and characterising the temporal changes of drifting subpulses from radio pulsars. The method was tested using simulated data as well as archived observations made with the Westerbork Synthesis Radio Telescope (WSRT) at wavelengths of 92 and 21 cm. Aims. The drifting subpulse phenomenon is a well known property of radio pulsars. It has been studied extensively since their discovery, however the properties of the temporal behaviour of drifting subpulses are not fully explored. The drifting can also be non-coherent and the presence of effects like nulling or drift rate changing can mask the drifting behaviour of the pulsar. The S2DFS is a robust method for investigating this phenomenon and by introducing it we aim to expand our knowledge of the temporal drifting subpulse properties. Methods. Our new analysis method uses horizonally collapsed fluctuation spectra obtained with the two-dimensional fluctuation spectrum (2DFS) method. Stacking the collapsed spectra obtained in a 256 pulse window which slides by a pulse at a time produces a map of the collapsed fluctuation spectrum (S2DFS plot). By analysing the maps one can easily determine the presence of any temporal drift changes. Results. Simulated data showed that the technique can reveal the presence of any temporal changes in drift behaviour like mode changing or nulling. We have also analysed data of three pulsars, PSRs B0031−07, B1819−22 and B1944+17, which were selected based on the quality of the data and their known drift properties. All three sources are known to exhibit mode changes which could easily be seen in the S2DFS. Conclusions. The results from the analysis of the data sets used in this paper have shown that the S2DFS method is robust and complimentary to the 2DFS method in detecting and characterising the temporal changes in drifting subpulses from radio pulsars.

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“…Alexeev et al (1969) and Vitkevich & Shitov (1970) are the first to detect the driftbands of 0809+74. Cole (1970) then notes that the driftrate of the subpulses occasionally changes, without being able yet to identify the nulls as the trigger. One year later, Taylor & Huguenin (1971) …”

Section: Introductionmentioning

confidence: 99%

Null-induced mode changes in PSR B0809+74

Leeuwen

Kouwenhoven

Ramachandran

et al. 2002

A&A

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Abstract. We have found that there are two distinct emission modes in PSR B0809+74. Beside its normal and most common mode, the pulsar emits in a significantly different quasi-stable mode after most or possibly all nulls, occasionally for over 100 pulses. In this mode the pulsar is brighter, the subpulse separation is less, the subpulses drift more slowly and the pulse window is shifted towards earlier longitudes. We can now account for several previously unexplained phenomena associated with the nulling-drifting interaction: the unexpected brightness of the first active pulse and the low post-null driftrate. We put forward a new interpretation of the subpulse-position jump over the null, indicating that the speedup time scale of the post-null drifting is much shorter than previously thought. The speedup time scale we find is no longer discrepant with the time scales found for the subpulse-drift slowdown and the emission decay around the null.

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Pulsar Sub-pulses and the Emission Process

Abstract: This article describes another regular phenomenon in the sub-pulse behaviour of pulsars. The drift speed of successive sub-pulses follows a sawtooth pattern with a linearly increasing drift speed and sudden jumps as the speed drops to repeat the cycle.

Cited by 21 publications

References 10 publications

PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

PSR B0809+74: Understanding its perplexing subpulse-separation (P$_\mathsf{2}$) variations

S2DFS: analysis of temporal changes of drifting subpulses

Null-induced mode changes in PSR B0809+74

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