Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

Li, L.; Wang, N.; Yuan, Jianping; Wang, J. B.; Hobbs, G.; Lentati, L.; Manchester, R. N.

doi:10.1093/mnras/stw1262

Cited by 14 publications

(17 citation statements)

References 40 publications

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“…By comparing with the earliest position reported by Johnston et al (1995), we obtain the proper motion with µ F α =−3(5) mas yr −1 and µ F δ =40(18) mas yr −1 . Table 3 lists the updated parameters for PSR J1733−3716, including its position, rotational frequency, frequency derivative and proper motion, which are consistent with previous measurements (Li et al 2016;Parthasarathy et al 2019).…”

Section: Timing Noise and Variations Of The Spin Parameterssupporting

confidence: 76%

“…This pulsar has a period derivative of 1.5×10 −14 s −2 , and characteristic age of 355 ky. Its integrated pulse profile has two peaks with the left peak being higher in intensity. Proper motion has been detected with value of µ α = 4(9) mas yr −1 and µ δ = 63(34) mas yr −1 (Li et al 2016). Recent work on PSR J1733−3716 has updated its position and rotation frequency parameters (Parthasarathy et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Timing and emission variation of PSR J1733−3716

Lin

Yuan

et al. 2020

Astrophys Space Sci

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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

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Section: Timing Noise and Variations Of The Spin Parameterssupporting

confidence: 76%

Section: Introductionmentioning

confidence: 99%

Timing and emission variation of PSR J1733−3716

Lin

Yuan

et al. 2020

Astrophys Space Sci

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“…Another mechanism is non-radial flow instabilities, such as convective overturn and the standing accretion shock instability (Foglizzo 2002;Blondin et al 2003;Foglizzo et al 2006Foglizzo et al , 2007Scheck et al 2008), which are able to produce asymmetric mass ejections during supernova explosions which can produce natal velocities from 100 km s −1 to up to and even beyond 1000 km s −1 . Next we explore the collision rate of asteroids on a pulsar with a pulsar velocity of 100 km s −1 (Blaes & Madau 1993;Ofek 2009;Li et al 2016). The low value leads to a larger cross section area for the collisions and hence the maximum value for the collision rate.…”

Section: Neutron Star Velocitymentioning

confidence: 99%

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

Smallwood

Martin

Zhang

2019

Monthly Notices of the Royal Astronomical Society

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The origin of fast radio bursts (FRBs) is still a mystery. One model proposed to interpret the only known repeating object, FRB 121102, is that the radio emission is generated from asteroids colliding with a highly magnetized neutron star (NS). With N -body simulations, we model a debris disc around a central star with an eccentric orbit intruding NS. As the NS approaches the first periastron passage, most of the comets are scattered away rather than being accreted by the NS. To match the observed FRB rate, the debris belt would have to be at least three orders of magnitude more dense than the Kuiper belt. We also consider the rate of collisions on to the central object but find that the density of the debris belt must be at least four orders of magnitude more dense than the Kuiper belt. These discrepancies in the density arise even if (1) one introduces a Kuiper-belt like comet belt rather than an asteroid belt and assume that comet impacts can also make FRBs; (2) the NS moves ∼ 2 orders of magnitude slower than their normal proper-motion velocity due to supernova kicks; and (3) the NS orbit is coplanar to the debris belt, which provides the highest rate of collisions.

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“…Desvignes et al 2016;Caballero et al 2016;Arzoumanian et al 2018). The results from Bayesian and frequentist methods have been compared and have shown to be generally consistent (for instance, Li et al 2016 andBabak et al 2016).…”

Section: Data and Processing For The Bayesian Analysismentioning

confidence: 99%

A pulsar-based time-scale from the International Pulsar Timing Array

Hobbs

Guo

Caballero

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We have constructed a new timescale, TT(IPTA16), based on observations of radio pulsars presented in the first data release from the International Pulsar Timing Array (IPTA). We used two analysis techniques with independent estimates of the noise models for the pulsar observations and different algorithms for obtaining the pulsar timescale. The two analyses agree within the estimated uncertainties and both agree with TT(BIPM17), a post-corrected timescale produced by the Bureau International des Poids et Mesures (BIPM). We show that both methods could detect significant errors in TT(BIPM17) if they were present. We estimate the stability of the atomic clocks from which TT(BIPM17) is derived using observations of four rubidium fountain clocks at the US Naval Observatory. Comparing the power spectrum of TT(IPTA16) with that of these fountain clocks suggests that pulsar-based timescales are unlikely to contribute to the stability of the best timescales over the next decade, but they will remain a valuable independent check on atomic timescales. We also find that the stability of the pulsar-based timescale is likely to be limited by our knowledge of solar-system dynamics, and that errors in TT(BIPM17) will not be a limiting factor for the primary goal of the IPTA, which is to search for the signatures of nano-Hertz gravitational waves.

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Proper motions of 15 pulsars: a comparison between Bayesian and frequentist algorithms

Cited by 14 publications

References 40 publications

Timing and emission variation of PSR J1733−3716

Timing and emission variation of PSR J1733−3716

Investigation of the asteroid–neutron star collision model for the repeating fast radio bursts

A pulsar-based time-scale from the International Pulsar Timing Array

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