Mode switching and oscillations in PSR B1828–11

Stairs, I. H.; Lyne, A. G.; Krämer, M.; Stappers, B. W.; Leeuwen, J. van; Tung, Alan; Manchester, R. N.; Hobbs, G.; Lorimer, D. R.; Melatos, A.

doi:10.1093/mnras/stz647

Cited by 36 publications

(26 citation statements)

References 62 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This can be done either for stars that show some periodic structure in their timing properties (see, e.g., Akgün et al 2006;Ashton et al 2017) or by assuming that some component of pulsar timing noise is due to precession (Cordes 1993). Note, however, that it is by no means clear whether pulsar timing really does provide evidence for free precession (Jones et al 2017;Stairs et al 2019).…”

Section: Signal Strengthmentioning

confidence: 99%

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data

Abbott¹,

Abbott²,

Abbott³

et al. 2019

ApJ

118

110

View full text Add to dashboard Cite

We present a search for gravitational waves from 222pulsars with rotation frequencies 10 Hz. We use advanced LIGO data from its first and second observing runs spanning 2015-2017, which provides the highest-sensitivity gravitational-wavedata so far obtained. In this search we target emission from both the l=m=2 mass quadrupole mode, with a frequency at twice that of the pulsar's rotation, and the l=2, m=1 mode, with a frequency at the pulsar rotation frequency. The search finds no evidence for gravitational-wave emission from any pulsar at either frequency. For the l=m=2 mode search, we provide updated upper limits on the gravitationalwave amplitude, mass quadrupole moment, and fiducial ellipticity for 167pulsars, and the first such limits for a further 55. For 20young pulsars these results give limits that are below those inferred from the pulsars' spin-down. For the Crab and Vela pulsars our results constrain gravitational-wave emission to account for less than 0.017%and 0.18%of the spin-down luminosity, respectively. For the recycled millisecond pulsar J0711 −6830our limits are only a factor of 1.3above the spin-down limit, assuming the canonical value of 10 38 kg m 2 for the star's moment of inertia, and imply a gravitational-wave-derived upper limit on the star's ellipticity of 1.2×10 −8. We also place new limits on the emission amplitude at the rotation frequency of the pulsars.

show abstract

Section: Signal Strengthmentioning

confidence: 99%

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data

Abbott¹,

Abbott²,

Abbott³

et al. 2019

ApJ

118

110

View full text Add to dashboard Cite

show abstract

“…This pulsar is notable for correlated profile and ν changes (Brook et al 2016. Stairs et al (2019) performed an exhaustive analysis on multi-hour long observations of this pulsar and reported that the pulsar undergoes mode-changing between two stable, extreme profile states. They stated that the observed mode transition rate can perhaps be explained by the chaotic behaviour model as previously suggested by Sey-mour & Lorimer (2013).…”

Section: Pulsars With Planetary Companions?mentioning

confidence: 99%

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Parthasarathy

Shannon

Johnston

et al. 2019

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

The smooth spin-down of young pulsars is perturbed by two non-deterministic phenomenon, glitches and timing noise. Although the timing noise provides insights into nuclear and plasma physics at extreme densities, it acts as a barrier to high-precision pulsar timing experiments. An improved methodology based on Bayesian inference is developed to simultaneously model the stochastic and deterministic parameters for a sample of 85 high-E radio pulsars observed for ∼ 10 years with the 64-m Parkes radio telescope. Timing noise is known to be a red process and we develop a parametrization based on the red-noise amplitude (A red ) and spectral index (β). We measure the median A red to be −10.4 +1.8 −1.7 yr 3/2 and β to be −5.2 +3.0 −3.8 and show that the strength of timing noise scales proportionally to ν 1 | ν| −0.6±0.1 , where ν is the spin frequency of the pulsar and ν its spin-down rate. Finally, we measure significant braking indices for 19 pulsars, proper motions for two pulsars and discuss the presence of periodic modulation in the arrival times of five pulsars.

show abstract

“…They found that the two stable states of this pulsar, namely normal mode and abnormal mode, account for 84.9 percent and 15.1 percent of the total duration, respectively. In the investigation of the young pulsar PSR B1828−11, it was revealed that the pulsar displays two stable modes, the wide mode and the narrow mode, with an estimation of around 500 days for the period of change between the two modes (Stairs et al 2019). Another phenomenon relates to pulse nulling, which could be regarded as an extreme mode changing, and demonstrates as disappearance of pulses for durations ranging from several pulse periods to many years (Wang et al 2007).…”

Section: Introductionmentioning

confidence: 99%

Timing and emission variation of PSR J1733−3716

Lin

Yuan

et al. 2020

Astrophys Space Sci

View full text Add to dashboard Cite

We present analysis of the timing noise in PSR J1733−3716, which combines data from Parkes 64-m radio telescope and nearly 15 years of timing data obtained from the Nanshan 25-m radio telescope. The variations in the spin frequency and frequency derivative are determined. The fluctuation in the spin frequency is obvious with an amplitude of 1.94(7)×10 −9 Hz. Variations of the integrated profile at 1369 MHz are detected with the changes occur in the relative peak intensity from the right profile component. From analysis of the single pulse data at 1382 MHz, we detect weak emission states that account for 63% of the whole data, and its duration distribution can be fitted with a power law. The pulsar also exhibits strong emission states, during which the emission shows multiple modes. This includes the normal mode, left mode and the right mode, with the time scales spanning between one and seventeen pulse periods. Such short term variability in pulses contributes to the variation of the integrated profile. Examination of the correlations between the spin parameters and the integrated profiles shows likelihood of a random distribution, which reveals that there is probably no obvious relationship between spin

show abstract

Mode switching and oscillations in PSR B1828–11

Cited by 36 publications

References 62 publications

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data

Searches for Gravitational Waves from Known Pulsars at Two Harmonics in 2015–2017 LIGO Data

Timing of young radio pulsars – I. Timing noise, periodic modulation, and proper motion

Timing and emission variation of PSR J1733−3716

Contact Info

Product

Resources

About