TMRT Observations of 26 Pulsars at 8.6 GHz

Zhao, Ru-Shuang; Wu, Xiaoguang; Yan, Zhen; Shen, Zhi-Qiang; Manchester, R. N.; Qiao, G. J.; Xu, R. X.; Wu, Yajun; Zhao, Rong-Bing; Li, Bin; Du, Y. J.; Lee, Kejia; Hao, Longfei; Liu, Qinghui; Lu, Jiguang; Shang, Lun-Hua; Wang, Jinqing; Wang, Min; Yuan, Jian; Zhi, Qi‐Jun; Zhong, Wang

doi:10.3847/1538-4357/aa8170

Cited by 14 publications

(18 citation statements)

References 71 publications

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“…Similar double peaked profiles with matching component separations are evident at higher frequencies for this pulsar (e.g. Kramer 1994;Zhao et al 2017, and references therein). However, as the signal-to-noise ratio (SNR) in the individual subbands is low, these reconstructed pulse shapes should be considered as first order estimates only.…”

Section: The Crab Pulsarsupporting

confidence: 72%

Probing Pulsar Scattering between 120 and 280 MHz with the MWA

Kirsten

Bhat

Meyers

et al. 2019

ApJ

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The high sensitivity and wide frequency coverage of the Murchison Widefield Array allow for the measurement of the spectral scaling of the pulsar scattering timescale, α, from a single observation. Here we present three case studies targeted at bright, strongly scattered pulsars J0534+2200 (the Crab pulsar), J0835−4510 (the Vela pulsar) and J0742−2822. We measure the scattering spectral indices to be −3.8 ± 0.2, −4.0 ± 1.5, and −2.5 ± 0.6 for the Crab, Vela, and J0742−2822, respectively. We find that the scattered profiles of both Vela and J0742−2822 are best described by a thin screen model where the Gum Nebula likely contributes most of the observed scattering delay. For the Crab pulsar we see characteristically different pulse shapes compared to higher frequencies, for which none of the scattering screen models we explore are found to be optimal. The presence of a finite inner scale to the turbulence can possibly explain some of the discrepancies.

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Section: The Crab Pulsarsupporting

confidence: 72%

Probing Pulsar Scattering between 120 and 280 MHz with the MWA

Kirsten

Bhat

Meyers

et al. 2019

ApJ

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“…The 5.0 GHz profile for this pulsar (Fig. 1) has a strong central (core) component with two equal outlier (conal) components on each side, similar to that at 8.6 GHz (Zhao et al 2017). At 1.4 and 3.1 GHz the central core component completely dominates the profile , consistent with the normally steeper spectral index for core emission.…”

Section: Normal Pulsarssupporting

confidence: 61%

“…The pulsars calibrated in this way are marked by a * in Table 1. For the other 41 pulsars which have no real-time flux density calibration, we estimated the mean flux density using the system equivalent flux density (cf., Zhao et al 2017), which is ≥ 26 Jy at 5.0 GHz (Wang et al 2015). From multiple observations of 3C123 we estimate a 20% calibration uncertainty.…”

Section: Resultsmentioning

confidence: 99%

“…Pulse widths at 50% and 10% of the profile maximum, W 50 and W 10 respectively, are also given in Table 1. Component separations and pulse widths were computed from fits of Gaussian profiles to components (cf., Zhao et al 2017). As for flux densities, for pulsars that were observed several times, mean widths and their uncertainties are given in Table 1.…”

Section: Resultsmentioning

confidence: 99%

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5.0 GHz TMRT Observations of 71 Pulsars

Zhao

Yan

et al. 2019

ApJ

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We present integrated pulse profiles at 5 GHz for 71 pulsars, including eight millisecond pulsars (MSPs), obtained using the Shanghai Tian Ma Radio Telescope (TMRT). Mean flux densities and pulse widths are measured. For 19 normal pulsars and one MSP, these are the first detections at 5 GHz and for a further 19, including five MPSs, the profiles have a better signal-to-noise ratio than previous observations. Mean flux density spectra between 400 MHz and 9 GHz are presented for 27 pulsars and correlations of power-law spectral index are found with characteristic age, radio pseudo-luminosity and spin-down luminosity. Mode changing was detected in five pulsars. The separation between the main pulse and interpulse is shown to be frequency independent for six pulsars but a frequency dependence of the relative intensity of the main pulse and interpulse is found. The frequency dependence of component separations is investigated for 20 pulsars and three groups are found: in seven cases the separation between the outmost leading and trailing components decreases with frequency, roughly in agreement with radius-to-frequency mapping; in eleven cases the separation is nearly constant; in the remain two cases the separation between the outmost components increases with frequency. We obtain the correlations of pulse widths with pulsar period and estimate the core widths of 23 multi-component profiles and conal widths of 17 multi-component profiles at 5.0 GHz using Gaussian fitting and discuss the width-period relationship at 5 GHz compared with the results at at 1.0 GHz and 8.6 GHz.

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“…As fossils of stellar evolution, radio pulsars are considered to be strongly gravitating, rapidly rotating, and strongly magnetized neutron stars (NSs), the products of massive stars evolving through supernova events. The spin periods of young radio pulsars have been observed to be decreasing (Liu et al ; Yan et al ; Zhao et al , ). A pulsar's secular spin‐down is probably caused by its rotational energy losses due to electromagnetic radiation, particle winds, intense neutrino emission, or gravitational radiation.…”

Section: Introductionmentioning

confidence: 99%

The evolution of magnetic field and spin‐down of young pulsars

2019

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Here, we summarize our recent work on the evolution of magnetic field and spin-down of young pulsars including high-B pulsars and magnetars. Our work includes the following three parts: (a) Based on the estimated ages of their potentially associated supernova remnants (SNRs), we estimate the values of the mean braking indices of eight magnetars with SNRs and find that five magnetars have smaller mean braking indices of 1 < n < 3, and we interpret them within a combination of magnetodipole radiation and wind-aided braking. (b) The low braking index of n = 0.9(2) for PSR J1734-3333 could undergo a supercritical accretion soon after its formation in a supernova explosion. The buried multipole magnetic fields will merge into a dipole magnetic field. Retaining the current field growth index = 1.34, this pulsar will become a magnetar with dB p ∼6.2(2) × 10 14 G and dB p ∼1.06(4) × 10 15 G after 50 kyrs and 100 kys, respectively. (c) By introducing a mean rotation energy conversion coefficient and combining the pulsar's high-energy and timing observations with a reliable nuclear equation of state, we estimate the initial spin period, initial dipole magnetic field, and true age of PSR J1640-4631. For this source, its measured high braking index n = 3.15(3) is attributed to a long-term dipole magnetic field decay, and its soft X-ray emission is attributed to anisotropic heating. K E Y W O R D SPSR J1640-4631, toroidal magnetic field, TPW heating

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TMRT Observations of 26 Pulsars at 8.6 GHz

Cited by 14 publications

References 71 publications

Probing Pulsar Scattering between 120 and 280 MHz with the MWA

Probing Pulsar Scattering between 120 and 280 MHz with the MWA

5.0 GHz TMRT Observations of 71 Pulsars

The evolution of magnetic field and spin‐down of young pulsars

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