Long-term observations of three nulling pulsars

Young, Neil J.; Weltevrede, P.; Stappers, B. W.; Lyne, A. G.; Krämer, M.

doi:10.1093/mnras/stv392

Cited by 29 publications

(32 citation statements)

References 50 publications

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“…Thus, more detailed observations of other intermediate nuller are needed to check if this property is shared by this class as a whole. PSRs B0823+26, J1634−5107 and PSR J1853+0505 all show weak emission during longer nulls (Young et al 2015), whereas we do not detect any weak emission in PSR B1706−16 after integrating all long nulls, although weak emission is seen for shorter nulls in AP. It may be noted that no weak emission was detected in the PSR J1717−4054 (Kerr et al 2014;Young et al 2015).…”

Section: Discussioncontrasting

confidence: 83%

“…PSRs B0823+26, J1634−5107 and PSR J1853+0505 all show weak emission during longer nulls (Young et al 2015), whereas we do not detect any weak emission in PSR B1706−16 after integrating all long nulls, although weak emission is seen for shorter nulls in AP. It may be noted that no weak emission was detected in the PSR J1717−4054 (Kerr et al 2014;Young et al 2015). Lastly, high timing noise or non-white timing residuals have been noted for PSR J1634−5107 and PSR J1717−4054, while such behaviour is not very apparent in PSR J1853+0505 and B0823+26.…”

Section: Discussioncontrasting

confidence: 83%

“…We also see evidence for such timing noise in our data. Such variableν was attributed to switching between distinct magnetospheric states for intermittent pulsars (Timokhin 2010 (Young et al 2015). It may be noted that these may be overestimates as the NF were mostly inferred from non-detection/detection statistics in these pulsars.…”

Section: Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Detection of long nulls in PSR B1706−16, a pulsar with large timing irregularities

Naidu

Joshi

Manoharan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Single pulse observations, characterizing in detail, the nulling behaviour of PSR B1706−16 are being reported for the first time in this paper. Our regular long duration monitoring of this pulsar reveals long nulls of 2 to 5 hours with an overall nulling fraction of 31±2%. The pulsar shows two distinct phases of emission. It is usually in an active phase, characterized by pulsations interspersed with shorter nulls, with a nulling fraction of about 15 %, but it also rarely switches to an inactive phase, consisting of long nulls. The nulls in this pulsar are concurrent between 326.5 and 610 MHz. Profile mode changes accompanied by changes in fluctuation properties are seen in this pulsar, which switches from mode A before a null to mode B after the null. The distribution of null durations in this pulsar is bimodal. With its occasional long nulls, PSR B1706−16 joins the small group of intermediate nullers, which lie between the classical nullers and the intermittent pulsars. Similar to other intermediate nullers, PSR B1706−16 shows high timing noise, which could be due to its rare long nulls if one assumes that the slowdown rate during such nulls is different from that during the bursts.

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Section: Discussioncontrasting

confidence: 83%

Section: Discussioncontrasting

confidence: 83%

See 1 more Smart Citation

Detection of long nulls in PSR B1706−16, a pulsar with large timing irregularities

Naidu

Joshi

Manoharan

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…At the same time, efforts are made toward finding similar spin down behaviours in nulling pulsars (e.g. a larger spin down rate when the pulsar is on [96]). Furthermore, rotating radio transients [58] and magnetar pulsed radio emission [10] were also discovered.…”

Section: Spin Down Of Intermittent Pulsarsmentioning

confidence: 99%

Pulsar braking: magnetodipole vs. wind

Tong

2015

Sci. China Phys. Mech. Astron.

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Pulsars are good clocks in the universe. One fundamental question is that why they are good clocks? This is related to the braking mechanism of pulsars. Nowadays pulsar timing is done with unprecedented accuracy. More pulsars have braking indices measured. The period derivative of intermittent pulsars and magnetars can vary by a factor of several. However, during pulsar studies, the magnetic dipole braking in vacuum is still often assumed. It is shown that the fundamental assumption of magnetic dipole braking (vacuum condition) does not exist and it is not consistent with the observations. The physical torque must consider the presence of the pulsar magnetosphere. Among various efforts, the wind braking model can explain many observations of pulsars and magnetars in a unified way. It is also consistent with the up-to-date observations. It is time for a paradigm shift in pulsar studies: from magnetic dipole braking to wind braking. As one alternative to the magnetospheric model, the fallback disk model is also discussed. Tong H. Pulsar braking: magnetodipole vs. wind.

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“…In fact, were the pulsar observed with a TOA precision of 1 ns, 33 per cent variations inν, occurring on a timescale of 2 hours would not be resolvable even when monitored almost continuously. No measurable ∆ν variations were detected in PSR J1853+0505 (Young et al 2015) which undergoes emission changes on timescales of just minutes. A TOA precision of 1 ns is required to resolve ∆ν = 1000 per cent or larger occurring on the same timescale.…”

Section: Pulsars With Known Variable Emissionmentioning

confidence: 91%

Resolving discrete pulsar spin-down states with current and future instrumentation

Shaw

Stappers

Weltevrede

2018

Monthly Notices of the Royal Astronomical Society

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An understanding of pulsar timing noise offers the potential to improve the timing precision of a large number of pulsars as well as facilitating our understanding of pulsar magnetospheres. For some sources, timing noise is attributable to a pulsar switching between two different spin-down rates (ν). Such transitions may be common but difficult to resolve using current techniques. In this work, we use simulations oḟ ν-variable pulsars to investigate the likelihood of resolving individualν transitions. We inject step-changes in the value ofν with a wide range of amplitudes and switching timescales. We then attempt to redetect these transitions using standard pulsar timing techniques. The pulse arrival-time precision and the observing cadence are varied. Limits onν detectability based on the effects such transitions have on the timing residuals are derived. With the typical cadences and timing precision of current timing programs, we find we are insensitive to a large region of ∆ν parameter space which encompasses small, short timescale switches. We find, where the rotation and emission states are correlated, that using changes to the pulse shape to estimateν transition epochs, can improve detectability in certain scenarios. The effects of cadence on ∆ν detectability are discussed and we make comparisons with a known population of intermittent and mode-switching pulsars. We conclude that for short timescale, small switches, cadence should not be compromised when new generations of ultra-sensitive radio telescopes are online.

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Long-term observations of three nulling pulsars

Cited by 29 publications

References 50 publications

Detection of long nulls in PSR B1706−16, a pulsar with large timing irregularities

Detection of long nulls in PSR B1706−16, a pulsar with large timing irregularities

Pulsar braking: magnetodipole vs. wind

Resolving discrete pulsar spin-down states with current and future instrumentation

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