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The follow-up timing observations were carried out for 24 pulsars discovered with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in Commensal Radio Astronomy FAST Survey. We report their phase-connected timing ephemeris, polarization pulse profiles, and Faraday rotation measurements. With their spin periods spanning from 2.995 ms to 4.34 s, their period derivatives were determined to spread between 7.996(8) × 10−21 and 9.83(3) × 10−15 s s−1, which imply that they have characteristic ages from 1.97 × 106 to 5.93 × 109 yr. It is inferred that PSRs J0211+4235 and J0518+2431 are beyond the ‘traditional death line’. PSR J0211+4235 is beyond the ‘death valley’. The death line model of Zhang et al. also cannot explain the radio presence of PSR J0211+4235. This suggests that radiation theory needs to be improved. Besides, ten of the 22 canonical pulsars show nulling phenomena. Moreover, PSR J1617+1123 exhibits variation of emission and J0540+4542 shows subpulse drifting. The DM of five pulsars is larger than the estimated by the YMW16 electron density model, which could suggest that electron density models need updates for higher Galactic latitude regions. PSRs J0447+2447 and J1928−0548 are isolated millisecond pulsars. With their flux densities spanning from 5(1)–553(106) μJy, some of these new pulsars found by FAST are distant, dim, and low-$\dot{E}$ ones and are suitable for testing pulsar emission theories.

We report the phase-connected timing ephemeris, polarization pulse profiles, Faraday rotation measurements, and Rotating-Vector-Model (RVM) fitting results of 12 millisecond pulsars (MSPs) discovered with the Five-hundred-meter Aperture Spherical radio Telescope (FAST) in the Commensal Radio Astronomy FAST survey (CRAFTS). The timing campaigns were carried out with FAST and Arecibo over 3 yr. 11 of the 12 pulsars are in neutron star–white dwarf binary systems, with orbital periods between 2.4 and 100 d. 10 of them have spin periods, companion masses, and orbital eccentricities that are consistent with the theoretical expectations for MSP–Helium white dwarf (He WD) systems. The last binary pulsar (PSR J1912−0952) has a significantly smaller spin frequency and a smaller companion mass, the latter could be caused by a low orbital inclination for the system. Its orbital period of 29 d is well within the range of orbital periods where some MSP–He WD systems have shown anomalous eccentricities, however, the eccentricity of PSR J1912−0952 is typical of what one finds for the remaining MSP–He WD systems.

We investigate properties of the low emission mode in PSR B0329+54 based on four single-pulse observations at frequency centred at 1.54 GHz using Nanshan radio telescope in Urumqi. The low emission mode is characterized by an intensity drop in the central component below that of the other two components. Referred here as the low mode, it has an average duration of 3P0 and is observed in both abnormal and normal emission modes of the pulsar occupying 3.6 per cent of the observed pulses. We demonstrate that the properties of low modes are related to the two modes. We find that the integrated profile of low modes is unique to the two modes, and that low modes occur more frequently when the pulsar is in the normal mode. Analysis of the energy distribution for normal low modes suggests that the cause for the intensity drop in the central component is separated from the emission of the other two components. We demonstrate that the pulse emission characteristics in the normal emission mode shortly after a low-mode bears some similarities with the abnormal mode and gradually recovering to the original normal emission in about three pulsar periods. In addition, the occurrence rate for low modes in different normal modes is mostly consistent, which implies that the duration of low modes is related to a normal mode for this pulsar. Our results imply profile modes each corresponds to specific magnetospheric plama density in particular geometric configuration, and profile mode changing signifies distinct changes of both at different parts of the profile.

We investigate the single-pulse emission variations of two pulsars, PSRs J0211+4235 and J0553+4111, observed with the Five-hundred-meter Aperture Spherical Radio Telescope at the 1.25 GHz central frequency. The observation sessions span from December 2020 to July 2021, with 21 and 22 observations for them. The integrated pulse profile of PSR J0211+4235 shows that there is a weak pulse component following the main component. And for PSR J0553+4111, it shows a bimodal profile with a bridge component in the middle. PSR J0211+4235 presents significant nulling phenomenon with nulling dura- tion lasting from 2 to 115 pulses and burst duration lasting from 2 to 113 pulses. The nulling fraction of each observation is determined to be 45% to 55%. No emission greater than three sigma is found in the mean integrated profile of all nulling pulses. In most cases, the pulse energy changes abruptly during the transition from null to burst, while in the transition from burst to null there are two trends: abrupt and gradual. We find that the nulling phenomenon of PSR J0211+4235 is periodic by Fourier transform of the null and burst state. In addition, the single-pulse modulation characteristics of these two pulsars are investigated, and the dis- tribution of modulation index, LRFS, 2DFS are analyzed with PSRSALSA. The left peak of PSR J0553+4111 has intensity modulation. Finally, the polarization property of these two pulsars are obtained through polarization calibration, and their characteristics are analyzed. The possible physical mechanisms of these phenomena are discussed.

We report the evolution of the X-ray pulsations of EXO 2030+375 during its 2021 outburst using the observations from Insight-HXMT. Based on the accretion torque model, we study the correlation between the spin frequency derivatives and the luminosity. Pulsations can be detected in the energy band of 1–160 keV. The pulse profile evolves significantly with luminosity during the outburst, leading to that the whole outburst can be divided into several parts with different characteristics. The evolution of the pulse profile reveals the transition between the supercritical (fan-beam dominated) and the subcritical accretion (pencil-beam dominated) mode. From the accretion torque model and the critical luminosity model, based on a distance of 7.1 kpc, the inferred magnetic fields are (0.41 − 0.74) × 1012 and (3.48 − 3.96) × 1012 G, respectively, or based on a distance of 3.6 kpc, the estimated magnetic fields are (2.4 − 4.3) × 1013 and (0.98 − 1.11) × 1012 G, respectively. Two different sets of magnetic fields both support the presence of multipole magnetic fields of the neutron star.

In this study, we report on a detailed single pulse analysis of the radio emission from the pulsar J1401$-$6357 (B1358$-$63) based on data observed with the ultrawideband low-frequency receiver on the Parkes radio telescope. In addition to a weak leading component, the integrated pulse profile features a single-humped structure with a slight asymmetry. The frequency evolution of the pulse profile is studied. Well-defined nulls, with an estimated nulling fraction greater than 2\%, are present across the whole frequency band. No emission is detected with significance above 3$\sigma$ in the average pulse profile integrated over all null pulses. Using fluctuation spectral analysis, we reveal the existence of temporal-dependent subpulse drifting in this pulsar for the first time. A clear double-peaked feature is present at exactly the alias border across the whole frequency band, which suggests that the apparent drift sense changes during the observation. Our observations provide further confirmation that the phenomena of pulse nulling and subpulse drifting are independent of observing frequency, which suggest that they invoke changes on the global magnetospheric scale., Comment: 10 pages, 13 figures

More than 50 years after the discovery of pulsars1 and confirmation of their association with supernova explosions2–4, the origin of the initial spin and velocity of pulsars remains largely a mystery. The typical space velocities of several hundred km s−1 have been attributed to ‘kicks’ resulting from asymmetries either in the supernova ejecta or in the neutrino emission5–7. Observations have shown a strong tendency for alignment between the pulsar space velocity and the spin axis in young pulsars, but until now these comparisons have been restricted to two dimensions. Here, we report evidence for three-dimensional alignment between the spin and velocity vectors, largely based on observations made with the Five-hundred-meter Aperture Spherical Radio Telescope (FAST) of the pulsar PSR J0538+2817 and its associated supernova remnant S147. Analysis of these and related observations has enabled us to determine the location of the pulsar within the supernova remnant and hence its radial velocity. Current simulations of supernova explosions have difficulty producing such three-dimensional alignment7–9. Our results, which depend on the unprecedented sensitivity of the observations, add another dimension to the intriguing correlation between pulsar spin-axis and birth-kick directions, thereby deepening the mysteries surrounding the birth of neutron stars. Fast-moving pulsars and neutron stars in general may have received a kinetic ‘kick’ from an asymmetric element in the supernova explosion that formed them. Here, the spin axis of a pulsar is determined to lie along the three-dimensional direction of the pulsar’s motion, providing a challenging constraint on supernova explosion modelling.

Obesity has become a global public health problem that seriously threatens population health. The Chinese government has attached great importance to prevent and control the negative impacts of obesity on individuals, families and society. China has established a policy system for obesity, and made certain achievements in behavioral intervention, drug treatment, traditional Chinese medicine treatment, and surgical treatment. This study summarizes the prevention and treatment experience of obesity in China in order to provide reference for African countries to better formulate prevention and treatment strategies for obesity in line with their local context.肥胖症已经成为严重威胁人类健康的全球公共卫生问题。如何防治肥胖症给个人、家庭和社会带来的危害已经引起中国政府的高度重视。中国针对肥胖症已建立了防治政策体系，并在行为干预、药物治疗、中医治疗、外科治疗等方面取得了一定的成效，现将中国对肥胖症的防治经验综述如下，以期为非洲各国更好地制定符合各国国情的肥胖症防治策略提供参考。.

In this study, we report on a detailed single pulse analysis of the radio emission from a rotating radio transient (RRAT) J1918$-$0449 which is the first RRAT discovered with the five hundred meter aperture spherical radio telescope (FAST). The sensitive observations were carried out on 30 April 2021 using the FAST with a central frequency of 1250 MHz and a short time resolution of 49.152 $\mu$s, which forms a reliable basis to probe single pulse emission properties in detail. The source was successively observed for around 2 hours. A total of 83 dispersed bursts with significance above 6$\sigma$ are detected over 1.8 hours. The source's DM and rotational period are determined to be 116.1$\pm$0.4 \pcm \ and 2479.21$\pm$0.03 ms, respectively. The share of registered pulses from the total number of observed period is 3.12\%. No underlying emission is detected in the averaged off pulse profile. For bursts with fluence larger than 10 Jy ms, the pulse energy follows a power-law distribution with an index of $-3.1\pm0.4$, suggesting the existence of bright pulse emission. We find that the distribution of time between subsequent pulses is consistent with a stationary Poisson process and find no evidence of clustering over the 1.8 h observations, giving a mean burst rate of one burst every 66 s. Close inspection of the detected bright pulses reveals that 21 pulses exhibit well-defined quasi-periodicities. The subpulse drifting is present in non-successive rotations with periodicity of $2.51\pm0.06$ periods. Finally, possible physical mechanisms are discussed., Comment: 11 pages, 11 figures

Biochar is a solid carbon material produced by heating organic biomass in the absence of oxygen through a process known as pyrolysis. Scientists and policy makers have recognised its potential role in carbon sequestration, reducing greenhouse gas emissions, renewable energy, waste mitigation and as soil amendment. To date, most studies related to biochar application to soil have focused mainly on the agronomic benefits, while little attention is paid on its effects on soil properties from geotechnical point of view. Considering that biochar can be produced from biomass, its use would fit satisfactorily the current trends of recycling wastes for ground improvement and liquefaction mitigation. To address this, the effect of adding various proportions by weight of biochar, derived from poultry litter, on the liquefaction resistance of sand is investigated through undrained cyclic triaxial tests. The findings suggest that, contrary to other earlier published reports using another type of biochar, adding poultry litter biochar to sand decreases its liquefaction resistance in a similar manner as adding non-plastic fines. The results highlight the fact that the type of biochar used as soil amendment is important in determining whether the liquefaction resistance of the host sand will improve or not.

The p-multiplier concept has been widely used to analyse the response of laterally loaded pile groups. Conventionally, the p-multiplier fm is evaluated iteratively by trial and error comparisons of p–y curves and field measurements. However, these approaches could face numerical difficulties and often require subjective adjustment and therefore could result in non-unique solutions. This paper derives a power relationship between fm and the force ratio at the pile head ηhead, defined by the ratio of the lateral force acting at the head of a group pile to that of a single pile, where ηhead equals fm to the power of n. In the case of long piles, it was found that (a) n = 3/4 when the initial modulus of subgrade reaction kini and the ultimate soil resistance pult are constant with depth; and (b) n = 3/5 when both kini and pult increase linearly with depth. This analytical relationship can then be utilised to determine fm from the test results of group piles and single piles, and quickly estimate the lateral bearing capacity of pile groups.

Expansive soils have been well recognised as problematic that can pose threats to the stability of the Earth's structures due to the soils’ significant volumetric change when subject to moisture variation. In this study, a modified oedometer set-up was used to investigate the one-dimensional swelling pressure of compacted soils when subject to wetting under the constant volume constraint. Four expansive residual soils found in Auckland, New Zealand were tested. Based on the findings of two soils, a prediction formula of the swelling pressure was proposed. The formula considers not only the initial condition of the soil but also implicitly the amount of swelling minerals through the material's free swell index. The formula was validated using swelling data obtained from the other two expansive soils tested in this study and from data reported in the literature. The predicted swelling pressure was found to be reasonably close to the measured pressure, considering the range of soil expansivity in this study.

Macroscopic mechanical properties of granular materials are closely related to particle morphology. For practical reasons, the morphological features are commonly examined from projected two-dimensional (2D) images of the three-dimensional (3D) particles. This brings forward the need for quantifying the correlations between the 2D and 3D particle descriptors. This paper addresses these correlations for irregular granular particles. Three-dimensional images of sand particles were acquired through microfocus X-ray computed tomography, based on which 3D surfaces of the particles were reconstructed using spherical harmonic analyses. The 3D particle size and shape descriptors were subsequently evaluated. All-around projection and random projection of the particles onto 2D planes were undertaken numerically to obtain the projected 2D images and thus the corresponding 2D size and shape descriptors. The results indicate that there are close correlations between 3D and 2D size descriptors averaged from the all-around projections. 2D and 3D shape descriptors can be approximately fitted with a linear relationship. The mean value of 2D descriptors of the tested sands obtained from a series of independent random-projection tests is essentially identical to that from the all-around projections; except that the data from the random-projection tests show a larger scatter. In light of the relationships among the descriptors, a novel and promising approach to predict the cumulative distribution of 3D descriptors from that of 2D descriptors evaluated from a random-projection test is proposed.

Vegetative porous concrete (VPC) could effectively reduce the adverse impacts of engineering construction on the environment and adapt to the demands of sustainable development. In this article, sh...

We presented observations of PSRs J0614+2229 and J1938+2213 using the Five-hundred-meter Aperture Spherical radio Telescope. PSR J0614+2229 shows two distinct emission states, in which the emission of state A occurs earlier than that of state B in longitude. The phase offset between the average pulse profile peaks of the two states is about 1.°05. The polarization properties of the average pulse profile of the two states are different with different linear position angle swings. We found that the emission becomes brighter during the transition between the two states, which has never been seen in other mode-changing pulsars before. PSR J1938+2213 appears to consist of a weak emission state superposed by brighter burst emissions. The weak state is always present and the energy of the strongest pulse in the burst state is about 57 times larger than that of the average pulse energy. The polarization properties of the two states are also different, and orthogonal polarization modes can be seen only in the burst state, rather than both states. Our results suggest that, for the two pulsars, the emissions of the two states may be generated in different regions in the pulsar magnetosphere.

In this paper, we investigate the emission properties of PSR J1727-2739, whose mean pulse profile has two main components, by analysing five single-pulse observations made using the Parkes 64-m radio telescope with a central frequency of 1369 MHz between 2014 April and October. The total observation time is about 6.1 hours which contains 16718 pulses after removal of radio frequency interference (RFI). Previous studies reveal that PSR J1727-2739 exhibits both nulling and subpulse drifting. We estimate the nulling fraction to be 66%, which is consistent with previously published results. In addition to the previously known subpulse drifting in the leading component, we also explore the drifting properties for the trailing component. We observe two distinct drift modes whose vertical drift band separations ($P_{3}$) are consistent with earlier studies. We find that both profile components share the same drift periodicity $P_{3}$ in a certain drift mode, but the measured horizontal separations ($P_{2}$) are quite different for them. That is, PSR J1727-2739 is a pulsar showing both changes of drift periodicity $P_{3}$ between different drift modes and drift rate variations between components in a given drift mode. Pulsars exhibiting nulling along with drift mode changing, such as PSR J1727-2739, give an unique opportunity to investigate the physical mechanism of these phenomena.

We report on the pulse-to-pulse energy distribution and longitude-resolved modulation properties of PSR J1631+1252 discovered by the Five-hundred-meter Aperture Spherical radio Telescope. Our analysis made use of the data acquired at 1250 MHz from the follow-up timing observations that lasted over a year. PSR J1631+1252 has a rotational period of ∼0.310 s, and a dispersion measure of ∼32.73 pc cm−3. The energy distribution is well described by a lognormal distribution, the parameters of which do not vary with time. We show that large modulation occurs across the bridge emission of the pulse profile, with sporadic bright bursts at the leading emission region. The fluctuation spectral analysis reveals the existence of subpulse drifting in the leading component with vertical spacing between the drift bands of 3.28 ± 0.08 pulse periods between consecutive drift bands. Possible physical mechanisms for subpulse drifting are discussed.

We report on the interstellar scintillation from pulsar J2048−1616 for the first time at 732, 1369, and 3100 MHz observed with the Parkes 64 m radio telescope. Dynamic spectra are obtained and diffractive parameters are derived from two-dimensional autocorrelation analyses. The frequency dependencies of the observed diffractive scintillation timescale and decorrelation bandwidth indicate that the electron density fluctuations in the interstellar medium (ISM) do not follow the Kolmogorov spectrum. The secondary spectra are calculated by forming the Fourier power spectra of the corresponding dynamic spectra. Prominent parabolic arcs are revealed in the secondary spectra at three frequencies, which indicate that they originated from scattering by a thin screen. The scattering screen is approximately located centrally between the pulsar and Earth assuming that the ISM is stationary.

Traditionally, the shape of a three-dimensional (3D) particle is inferred from a single parameter called the aspect ratio (AR) that is evaluated from a collection of projected two-dimensional (2D) images of the 3D particle. While this approach could offer an estimate of the particle shape, it is likely that a single parameter is insufficient to describe the 3D shape characteristics of a particle. Conventionally, the shape of a 3D particle can be described by two parameters: the elongation index (EI) and the flatness index (FI), defined as the length ratios of different principal dimensions. This paper presents a novel approach that can be used to evaluate the EI and FI of 3D particles based on their projected 2D images. The novelty of this proposed method is that the distribution of the AR is considered rather than only the mean value. The performance of the algorithm is examined using numerically generated ellipsoids and real sand particles scanned using microfocus X-ray computed tomography. The results appear promising and the plausible combinations of the EI and FI of the 3D particles can be obtained.

This paper investigates the relationship between the 3D size and shape characteristics of ellipsoids and their 2D counterparts obtained from projected images. We found that the average radius of ellipsoids can be satisfactorily estimated from the statistical mean or median of the average radius of the corresponding 2D projected images. However, the shape characteristics evaluated from the images may not always yield reliable quantitative prediction of the corresponding 3D descriptors. The results suggest that quantifying particle shape characteristics from projected 2D images may only work well for particles similar in shape to prolate spheroids.

This paper presents nondimensional solutions and parametric studies of the responses of laterally loaded piles in overconsolidated clay. Nondimensional expressions of a nonlinear p-y model, termed as the H-model, and the governing equation of laterally loaded piles were derived and solved. Parametric studies by virtue of the nondimensional solutions were conducted, which revealed that the pile head response is highly sensitive to the change in the soil undrained shear strength (su), the maximum lateral bearing factor (np(max)), and the ratio of the elastic modulus of subgrade reaction to the soil undrained shear strength (nk), but is insensitive to other parameters in the model.

We have carried out a detailed study of single-pulse emission from the pulsar J2048−1616 (B2045−16), observed at 732, 1369, and 3100 MHz frequencies using the Parkes 64 m radio telescope. The pulsar possesses three well-resolved emission components, with the central component resembling core emission. The single pulses show the presence of two distinct periodic modulations using fluctuation spectral analysis. About 12% nulls are found to create alternating bunches of nulls and bursts in a quasiperiodic manner with longer periodicities of 83, 28, and 14 rotational periods for simultaneous observations at 732 and 3100 MHz. At 1369 MHz, the quasiperiodic nulling is detected, as well, to modulate across the entire profile both in the core and conal components simultaneously with a fluctuation rate of about 50 rotational periods, and the nulling fraction is estimated to be around 10%. Additionally, the quasiperiodic modulations are significantly dependent on time. In addition to nulling, the pulsar also presents subpulse drifting in the single-pulse sequences with shorter periodicity. The subpulse drifting is presented in the conal components and is absent in the central core emission. The leading component is modulated in longitude with a period of three pulses. The trailing component remains phase stationary within the pulse window but periodically modulates in amplitude with a period of three pulses. Finally, possible physical mechanisms are discussed.

Particle angularity significantly affects the macroscopic mechanical behavior of aggregate assemblages. However, most of the current approaches used for quantifying particle angularity are only applicable to star-like particles. This study presents a new approach allowing the quantification of angularity of general-shape particles. The method first reconstructs the particle morphology by applying Fourier series analysis to the two-dimensional image of the particle. The gradient-based angularity index (AIg) is then evaluated from the reconstructed morphology through numerical integration. AIg is zero for images of any circularly shaped particles, including circles and ellipses, and it increases with increasing particle angularity. Images included in commonly used standard charts are evaluated for their AIgs. The results show a consistent pattern in regard to the qualitative angularity ranking of the particles. Based on the findings, a simple-to-use criterion is suggested for the quantitative classification of particle angularity.

The morphological features of sand particles play a key role in the mechanical response of the particle assemblage. Advancement of microfocus X-ray computed tomography (μXCT) technology has enabled 3D visualization of particles at the grain-scale with reasonably high resolution to reveal the particle morphology. This paper utilizes the real part of spherical harmonic (SH) functions to describe the morphology of general-shape sand particles acquired from μXCT images. The influence of the maximum degree of SH functions and mesh fineness on the determination of size and shape descriptors of the particles are systematically investigated. Correlations between different shape descriptors of the studied sands are examined. Utilizing principal component analysis (PCA) and the empirical cumulative distribution function (ECDF), a probabilistic approach considering both intrinsic and phenomenological correlations between SH coefficients is proposed to three-dimensionally regenerate the sand particles. Based on comprehensive and quantitative comparisons between the morphological characteristics of scanned and generated particles, we conclude that the proposed approach performs satisfactorily.

We present here the analysis of giant micropulses from the Vela pulsar. A total of 4187 giant micropulses with peak flux density $>$2.5 Jy were detected during almost 4 hours of observations carried out with the Yunnan 40-m radio telescope at 6800 MHz. Nine of the giant micropulses arrived approximately 3 to 4 ms earlier than the peak of average pulse profile, longer than that at lower frequencies. The remaining giant micropulses were clustered into three distributions which correspond to three main emission regions, including four occurring on the trailing edge of averaged profile., 9 pages, 8 figures

Glitches correspond to sudden jumps of rotation frequency ($\nu$) and its derivative ($\dot{\nu}$) of pulsars, the origin of which remains not well understood yet, partly because the jump processes of most glitches are not well time-resolved. There are three large glitches of the Crab pulsar, detected in 1989, 1996 and 2017, which were found to have delayed spin-up processes before the normal recovery processes. Here we report two additional glitches of the Crab pulsar occurred in 2004 and 2011 for which we discovered delayed spin up processes, and present refined parameters of the largest glitch occurred in 2017. The initial rising time of the glitch is determined as $, Comment: 25 pages, 8 figures

We report the emission variations in PSR J1047$-$6709 observed at 1369 MHz using the Parkes 64 m radio telescope. This pulsar shows two distinct emission states: a weak state and a bright emission state. We detected giant pulses (GPs) in the bright state for the first time. We found 75 GPs with pulse width ranging from 0.6 to 2.6 ms. The energy of GPs follows a power-law distribution with the index $\alpha=-3.26\pm0.22$. The peak flux density of the brightest GP is 19 Jy which is 110 times stronger than the mean pulse profile. The polarization properties of the average profile of GPs are similar to that of the pulses with energy less than 10 times average pulse energy in the bright state. This indicates that the emission mechanism is basically the same for them. Our results provide a new insight into the origin of the GPs in pulsars., Comment: 6 pages, 5 figures, Accepted for publication in MNRAS

By analysing the data acquired from the Parkes 64-m radio telescope at 1369 MHz, we report on the phase-stationary non-drift amplitude modulation observed in PSR J1048-5832. The high-sensitivity observations revealed that the central and trailing components of the pulse profile of this pulsar switch between a strong mode and a weak mode periodically. However, the leading component remains unchanged. Polarization properties of the strong and weak modes are investigated. Considering the similarity to mode changing, we argue that the periodic amplitude modulation in PSR J1048$-$5832 is periodic mode changing. The fluctuation spectral analysis showed that the modulation period is very short (~2.1 s or 17 P1), where P1 is the rotation period of the pulsar. We find that this periodic amplitude modulation is hard to explain by existing models that account for the periodic phenomena in pulsars like subpulse drifting., 8 pages, 8 figures, 3 tables, accepted in MNRAS for publication

Fast radio bursts (FRBs) are millisecond-duration radio transients of unknown origin. Two possible mechanisms that could generate extremely coherent emission from FRBs invoke neutron star magnetospheres or relativistic shocks far from the central energy source. Detailed polarization observations may help us to understand the emission mechanism. However, the available FRB polarization data have been perplexing, because they show a host of polarimetric properties, including either a constant polarization angle during each burst for some repeaters or variable polarization angles in some other apparently one-off events. Here we report observations of 15 bursts from FRB 180301 and find various polarization angle swings in seven of them. The diversity of the polarization angle features of these bursts is consistent with a magnetospheric origin of the radio emission, and disfavours the radiation models invoking relativistic shocks., Published online in Nature on 29 Oct, 2020

We present a detailed single-pulse analysis for PSR B1929+10 based on observations with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The main pulse and interpulse are found to be modulated with a periodicity of $\sim12$ times the pulsar's rotational period ($P$). The $\sim12P$ modulation is confirmed as a periodic amplitude modulation instead of systematic drifting. The periodic amplitude modulation in the IP is found to be anti-correlated with that in the weak preceding component of the MP (MP_I), but correlated with that in the first two components of the MP (MP_II), which implies that the modulation patterns in the IP and the MP are phase-locked. What is more interesting is that the modulation in MP_II is delayed that in the IP by about 1P. Furthermore, high sensitivity observations by FAST reveal that weak emission exists between the MP and the IP. In addition, we confirm that the separation between the IP and the MP is independent of radio frequency. The above results are a conundrum for pulsar theories and cannot be satisfactorily explained by the current pulsar models. Therefore, our results observed with FAST provide an opportunity to probe the structure of pulsar emission and the neutron star's magnetosphere., Comment: 13 pages 12 figures

Pulse arrival time measurements over fourteen years with the Nanshan 25-m and Parkes 64-m radio telescopes have been used to determine the average profile and timing properties for PSR J1757$-$2421 (B1754$-$24). Analysis of the radio profile data shows a large variation of spectral index across the profile and an unusual increase in component separation with increasing frequency. The timing observations show that PSR B1754$-$24 underwent a large glitch with a fractional increase in spin frequency of $\Delta\nu_{\rm g}/\nu\sim 7.8\times10^{-6}$ in May 2011. At the time of the glitch there was a large permanent jump in the rotational frequency accompanied by two exponential recovery terms with timescales of 15(6) and 97(15) days, respectively., Comment: 9 pages, 8 figures, 5 tables, Accepted for publication in MNRAS

In order to study the primary and secondary relationship between the factors affecting the engraving resistance of one small-caliber rifle projectile, quasi-static push tests were carried out for jacket material by H90 copper and copper clad steel projectile in three kinds of gun barrels with different structures and the corresponding changes of the engraving resistance were obtained and analyzed. At the same time, numerical simulations were carried out for constant high-speed extrusion. Quasi-static test and dynamic simulation results were analyzed, the order of the factors affecting the peak of engraving resistance under quasi-static is the yield strength of jacket>free stroke> engraving length>rifle number> lead, and the factors affecting the peak of extrusion force under high-speed is engraving velocity>yield strength of jacket>free stroke> engraving length >rifle number>lead. It is also found that the relative steady engraving resistance value is close 60% of its peak value under quasi-static, while the same value under high-speed is between 1/8 and 1/6 of the peak value, the results of force peak are basically quite.