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Pulsar's position, proper motion and parallax are important parameters in timing equations. It is a really challenging work to fit astrometric parameters accurately through pulsar timing, especially for pulsars that show irregular timing properties. As the fast development of related techniques, it is possible to measure astrometric parameters of more and more pulsars in a model$\textrm{-}$independent manner with the Very Long Baseline Interferometry (VLBI). In this work, we select 16 normal pulsars, whose parallax and proper motion have not been successfully fitted with timing observations or show obvious differences with corresponding latest VLBI solutions, and do further studies on their timing properties. After updating astrometric parameters in pulsar ephemerides with the latest VLBI measurements, we derive the latest rotation solutions of these pulsars with observation data at S and C$\textrm{-}$band obtained from the Shanghai Tian Ma Radio Telescope (TMRT). Compared with spin frequency $\nu$ inferred from previous rotation solutions, the newly$\textrm{-}$fitted $\nu$ show differences larger than 10$^{-9}$ Hz for most pulsars. The contribution of the Shklovsky effect to period derivative $\dot{P}$ can be properly removed taking advantages of accurate proper motion and distance of target pulsars measured by VLBI astrometry. This further leads to a precise estimate of intrinsic characteristic age $\tau_{\rm c}$. Differences between the newly$\textrm{-}$measured $\tau_{\rm c}$ and corresponding previous results are as large as 2% for some pulsars. VLBI astrometric parameter solutions also lead to better measurements of timing irregularities. For PSR B0154$+$61, the glitch epoch (MJD 58279.5) measured with previous ephemeris is about 13 d later than the result (MJD 58266.4) obtained with VLBI astrometric parameter solutions.

One large glitch was detected in PSR B1737$-$30 using data spanning from MJD 57999 to 58406 obtained with the newly built Shanghai Tian Ma Radio Telescope (TMRT). The glitch took place at the time around MJD 58232.4 when the pulsar underwent an increase in the rotation frequency of $\Delta \nu$ about 1.38$\times 10^{-6}$ Hz, corresponding to a fractional step change of $\Delta \nu / \nu$ $\thicksim$ 8.39$\times 10^{-7}$. Post$\textrm{-}$glitch $\nu$ gradually decreased to the pre$\textrm{-}$glitch value. The frequency derivative was observed to undergo a step change of about $-$9$\times 10^{-16}$ s$^{-2}$. Since July 1987, there are 36 glitches already reported in PSR B1737$-$30 including this one. According to our analysis, the glitch size distribution is well described by the power law with index of 1.13. The distribution of the interval between two adjacent glitches (waiting time $\Delta T$) follows a Poissonian probability density function. For PSR B1737$-$30, the interval is prone to be long after a large glitch. But no correlation is found between glitch size and the interval since previous glitch., Comment: 12 papges, 7 figures

We have investigated the mode-changing properties of PSR B0329+54 using 31 epochs of simultaneous 13 cm/3 cm single-pulse observations obtained with Shanghai Tian Ma 65 m telescope. The pulsar was found in the abnormal emission mode 17 times, accounting for ~13% of the 41.6 hours total observation time. Single pulse analyses indicate that mode changes took place simultaneously at 13 cm/3 cm within a few rotational periods. We detected occasional bright and narrow pulses whose peak flux densities were 10 times higher than that of the integrated profile in both bands. At 3 cm, about 0.66% and 0.27% of single pulses were bright in the normal mode and abnormal mode respectively, but at 13 cm the occurrence rate was only about 0.007%. We divided the pulsar radiation window into three components (C1, C2 and C3) corresponding to the main peaks of the integrated profile. The bright pulses preferentially occurred at pulse phases corresponding to the peaks of C2 and C3. Fluctuation spectra showed that C2 had excess red noise in the normal mode, but broad quasi-periodic features with central frequencies around 0.12 cycles/period in the abnormal mode. At 3 cm, C3 had a stronger quasi-periodic modulation centered around 0.06 cycles/period in the abnormal mode. Although there were some asymmetries in the two-dimensional fluctuation spectra, we found no clear evidence for systematic subpulse drifting. Consistent with previous low-frequency observations, we found a very low nulling probability for B0329+54 with upper limits of 0.13% and 1.68% at 13 cm/3 cm respectively., Comment: 16 pages, 10 figures, 3 tables

The emission geometries, e.g. the emission region height, the beam shape, and radius-to-frequency mapping, are important predictions of pulsar radiation model. The multi-band radio observations carry such valuable information. In this paper, we study two bright pulsars, (PSRs B0329+54 and B1642-03) and observe them in high frequency (2.5 GHz, 5 GHz, and 8 GHz). The newly acquired data together with historical archive provide an atlas of multi-frequency profiles spanning from 100 MHz to 10 GHz. We study the frequency evolution of pulse profiles and the radiation regions with the these data. We firstly fit the pulse profiles with Gaussian functions to determine the phase of each component, and then calculate the radiation altitudes of different emission components and the radiation regions. We find that the inverse Compton scattering (ICS) model can reproduce the radiation geometry of these two pulsars. But for PSR B0329+54 the radiation can be generated in either annular gap (AG) or core gap (CG), while the radiation of PSR B1642-03 can only be generated in the CG. This difference is caused by the inclination angle and the impact angle of these two pulsars. The relation of beaming angle (the angle between the radiation direction and the magnetic axis) and the radiation altitudes versus frequency is also presented by modelling the beam-frequency evolution in the ICS model. The multi-band pulse profiles of these two pulsars can be described well by the ICS model combined with the CG and AG.

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.

Integrated pulse profiles at 8.6~GHz obtained with the Shanghai Tian Ma Radio Telescope (TMRT) are presented for a sample of 26 pulsars. Mean flux densities and pulse width parameters of these pulsars are estimated. For eleven pulsars these are the first high-frequency observations and for a further four, our observations have a better signal-to-noise ratio than previous observations. For one (PSR J0742-2822) the 8.6~GHz profiles differs from previously observed profiles. A comparison of 19 profiles with those at other frequencies shows that in nine cases the separation between the outmost leading and trailing components decreases with frequency, roughly in agreement with radius-to-frequency mapping, whereas in the other ten the separation is nearly constant. Different spectral indices of profile components lead to the variation of integrated pulse profile shapes with frequency. In seven pulsars with multi-component profiles, the spectral indices of the central components are steeper than those of the outer components. For the 12 pulsars with multi-component profiles in the high-frequency sample, we estimate the core width using gaussian fitting and discuss the width-period relationship., Comment: 33 pages, 49 figures, 5 Tables; accepted by ApJ

The spatial distributions of old neutron stars (NSs) with ages 109 to 1010 yr in our Galaxy are investigated byMonte Carlo simulation under two different initial random velocity models. It is found that the scale heights of the distribution increase with the Galactic radial distance. The location of the peak of the NS distribution is closer to the Galactic center than that of their progenitors. The results from our detailed numerical analysis reveal that there is resemblance between the simulated old NS distribution and the structure of the observed HI disk.

In this paper, we discuss a rigorous treatment of the refractive scintillation caused by a two-component interstellar scattering medium and a Kolmogorov form of density spectrum. It is assumed that the interstellar scattering medium is composed of a thin-screen interstellar medium (ISM) and an extended interstellar medium. We consider the case that the scattering of the thin screen concentrates in a thin layer represented by a δ function distribution and that the scattering density of the extended irregular medium satisfies the Gaussian distribution. We investigate and develop equations for the flux density structure function corresponding to this two-component ISM geometry in the scattering density distribution and compare our result with the observations. We conclude that the refractive scintillation caused by this two-component ISM scattering gives a more satisfactory explanation for the observed flux density variation than does the single extended medium model. The level of refractive scintillation is strongly sensitive to the distribution of scattering material along the line of sight (LOS). The theoretical modulation indices are comparatively less sensitive to the scattering strength of the thin-screen medium, but they critically depend on the distance from the observer to the thin screen. The logarithmic slope of the structure function is sensitive to the scattering strength of the thin-screen medium, but is relatively insensitive to the thin-screen location. Therefore, the proposed model can be applied to interpret the structure functions of flux density observed in pulsar PSR B2111 + 46 and PSR B0136 + 57. The result suggests that the medium consists of a discontinuous distribution of plasma turbulence embedded in the interstellar medium. Thus our work provides some insight into the distribution of the scattering along the LOS to the pulsar PSR B2111 + 46 and PSR B0136 + 57.

Based on the undisturbed, finite thickness disk gravitational potential, we carried out 3-D Monte Carlo simulations of normal pulsars. We find that their scale height evolves in a similar way for different velocity dispersions (sigma(nu)): it first increases linearly with time, reaches a peak, then gradually decreases, and finally approaches a stable asymptotic value. The initial velocity dispersion has a very large influence on the scale height. The time evolution of the scale height is studied. When the magnetic decay age is used as the time variable, the observed scale height has a similar trend as the simulated results in the linear stage, from which we derive velocity dispersions in the range 70 similar to 178 km s(-1), which are near the statistical result of 90 similar to 270 km s(-1) for 92 pulsars with known transverse velocities. If the characteristic age is used as the time variable, then the observed and theoretical curves roughly agree for t > 10(8) yr only if sigma(nu) < 25 km s(-1).

Using the method of Gaussian Fit Separation of Average Profile (GFSAP), we re-examine the average profiles of nine pulsars at several frequencies, ranging from 408–1642 MHz. This method enables us to obtain the number of components for each pulsar, and the parameters for each component, the width, position and amplitude. The ρ-P relation for the inner cone and outer cone are studied separately, and the results are, respectively, ρ = P−0.51±0.05 and ρ = P−0.42±0.06. The results can be interpreted as a confirmation of the double-cone structure of pulsar emission beams. The altitudes of emission region, and the radius-to-frequency-map (RFM) are also examined; for the outer cone, we obtained r(v) ∝ v−0.19±0.09.

The initial period of a pulsar is an important factor in our understanding of the formation of neutron stars and of the nature of the equation of state of neutron star matter. Up to now this quantity can only be obtained for a few pulsars for which accurate age and braking index are known. Based on the theory of the off-center dipole emission, in which pulsars obtain their high velocities depending on the initial periods, we calculate the initial period using the proper motion data. Because the orbital velocity of the progenitor and asymmetric kick in the supernova explosion may also contribute to the observed velocity of the pulsar, the derived values of initial periods are lower limits. For normal pulsars, the initial periods are in the range of 0.6 similar to 2.6 ms. For the millisecond pulsars, the initial periods are comparable to their current periods, and the ratio between the initial period and the current period increases with the decrease of the current period. For PSR B1937+21 with the shortest period of 1.56 ms, the ratio is 0.77.

We present the status and results of pulsar observations in China. Pulsar observations at Urumqi Observatory over more than two years have resulted in updated rotation parameters for 74 pulsars. Comparison with earlier observations shows that long-term period and period-derivative fluctuations are probably dominated by unseen glitches. We also monitored the variation of pulsar scintillation dynamic spectra for a few strong pulsars. The data show major variations in the scintillation parameters. A new system at a lower frequency is planned to allow investigation of the frequency dependence of pulsar properties. A 50-m telescope for millisecond pulsar timing is also being planned at the National Astronomical Observatories, Beijing, and should be constructed within three years.

In this paper, we report radio observations of the Galactic Center magnetar PSR J1745-2900 at six epochs between June and October, 2014. These observations were carried out using the new Shanghai Tian Ma Radio Telescope at a frequency of 8.6 GHz. Both the flux density and integrated profile of PSR J1745-2900 show dramatic changes from epoch to epoch showing that the pulsar was in its "erratic" phase. On MJD 56836, the flux density of this magnetar was about 8.7 mJy, which was ten times large than that reported at the time of discovery, enabling a single-pulse analysis. The emission is dominated by narrow "spiky" pulses which follow a log-normal distribution in peak flux density. From 1913 pulses, we detected 53 pulses whose peak flux density is ten times greater than that of the integrated profile. They are concentrated in pulse phase at the peaks of the integrated profile. The pulse widths at the 50% level of these bright pulses was between 0.2 to 0.9 deg, much narrower than that of integrated profile (~12 deg). The observed pulse widths may be limited by interstellar scattering. No clear correlation was found between the widths and peak flux density of these pulses and no evidence was found for subpulse drifting. Relatively strong spiky pulses are also detected in the other five epochs of observation, showing the same properties as that detected in MJD 56836. These strong spiky pulses cannot be classified as "giant" pulses but are more closely related to normal pulse emission., Comment: 21 papes, 7 figures, accepted by ApJ

An important parameter in the study of the radial structure of the pulsar radio emission region is the altitude of the emission, but this cannot be derived directly from the observations. The altitude can be expressed as a function of frequency, ; r ν p ν -ξ , and the method of K analysis can be used to calculate the power law index ξ for 18 pulsars observed at two frequencies, 610 MHz and 1408 MHz and for three pulsars observed at three or more frequencies. The average value of ξ is 0.27, which indicates that the emission altitude increases with decreasing frequency and that the radial structure is compact.

A pulsar timing system has been operating in the 18-cm band at the Urumqi Astronomical Observatory 25-m telescope since mid-1999. Frequency resolution allowing dedispersion of the pulsar signals is provided by a 2X128X2.5 MHz filterbank/digitiser system. Observations of 74 pulsars over more than 12 months have resulted in updated pulsar periods and period derivatives, as well as improved positions. Comparison with previous measurements showed that the changes in period and period derivative tend to have the same sign and to be correlated in amplitude. A model based on unseen glitches gives a good explanation of the observed changes, suggesting that long-term fluctuations in period and period derivatives are dominated by glitches. In 2000 July, we detected a glitch of relative amplitude Delta_nu/nu~24X1e-9 in the Crab pulsar. The post-glitch decay appears similar to other large Crab glitches., Comment: 11 pages, 9 figures, 4 tables, accepted by MNRAS

Radio observational results at 232 MHz and multifrequency studies of the supernova remnant (SNR) HB21 are presented. Its integrated flux density at 232 MHz is about 390 ± 30 Jy. Both the integrated spectral index and the spatial variations of spectral index of the remnant were calculated by combining the new map at 232 MHz with previously published maps made at 408, 1420, 2695, and 4750 MHz. The SNR has an integrated spectral index of about α = −0.43 (Sν ∝ να) between 232 and 4750 MHz. In general the spectral index varies from −0.5 in southeast and west regions of the remnant to–0.3 in the central region and near the northwest edge. The new data of 232 MHz reveal that there is interaction between the remnant and the surrounding gas along the east edge of the remnant which causes the spectrum flattening at low frequency, while the very good agreement between the structure of X-ray emission and the central flat spectrum area suggests that the existence of thermal emission is the reason of spectrum flattening in the area.

Using a new pulsar timing system at the 25-m radio telescope of Urumqi Astronomical Observatory, we have detected a large glitch in the Crab pulsar which occurred in 2000 July. The size of the glitch is Deltav/v similar to 2.4 x 10(-8), with a relative increment in frequency derivative Delta (v) overdot / (v) over dot similar to 5 x 10(-3). The observing system is introduced and the observed properties of the glitch axe discussed.

According to the observational limits on the radius and mass, the fastest rotating pulsar (PSR 1937+21) is probably a strange star, or at least some neutron star equations of state should be ruled out, if we suggest that a dipole magnetic field is relevant to its radio emission. We presume that the millisecond pulsar is a strange star with {\em much} low mass, small radius, and weak magnetic moment., 9 pages, 2 figures, 1 table, to be published in Chinese Physics Letters (2001), http://vega.bac.pku.edu.cn/~rxxu

Scintillation of pulsar radio emission provides information about the interstellar medium along the path to the pulsar and the velocities of pulsars. It also affects the precision of pulse timing observations. Using a pulsar timing system developed at the Urumqi Astronomical Observatory 25 m telescope, we observed diffractive scintillation dynamic spectra for several strong northern pulsars. This paper introduces the observing system and discusses the observational results.

This paper presents a mathematical method for de-dispersion of average pulsar profiles. We applied this method to four dispersed pulsar profiles. The results revealed that this method significantly removed the dispersion broadening and the pulse widths were reduced by about 7% to 27%, depending on the magnitude of the pulsar dispersion measure.

We present the results of observations of the pulsar PSR B0329+54 at 0.327, 1.5, 2.3, 4.8 and 8.4 GHz during 1999 between 03-12 and 06-08, using the 25-m radio telescope of NAOC Urumqi Station. The spectrum shows a bend, the spectral index is 1.59 at the low frequency end, and 2.45 at the high frequency end. The angular width of the average pulse profile and the angular separation between two weak peaks both decrease with increasing frequency.

A flux density variation event in PSR B0809+74 over some 11 hours is presented. This event was discovered during our routine monitoring of pulsars at 327 MHz using the 25-m radio telescope of Urumqi Astronomical Observatory. The observed time scale of variation is rather different from both the time scales of diffractive and refractive interstellar scintillation. This event may be due to a new propagation effect.

Based on the undisturbed finitely thick disk gravitational potential, 3-D trajectories of pulsars are followed with initial locations and velocities randomly selected from a model distribution. Three typical instances are followed for some 10 11 yr, and their Poincare sections are used as diagnostics of their motion. We find that the vertical-to-parallel range ratio (relative to the Galactic plane) to be an important parameter: as this ratio increases, the pulsar's motion changes from being regular to being irregular/chaotic.

We use the cyclotron-maser theory to explain the core emission from the magnetosphere of pulsars. As a kind of direct and efficient maser type of emission, it can give rise to escaping radiation with extremely high brightness temperature and narrow angle with respect to the magnetic axis. We find that the growth rates and real frequencies of the O-mode electromagnetic wave propagating parallel to the magnetic fields depend on the ratio of the plasma frequency $\omega_p$ and the gyrofrequency $\omega_b$ rather than the plasma frequency alone, as described by other models. The emission takes place in the region where the magnitude of $\omega_p/\omega_b$ is $10^{-2}$. The corresponding altitude is about a few decades of neutron star radius, where the magnetic field strength is about $10^6-10^8 G$. The qualitative spectrum and the lower frequency cut-off of the radio emission is obtained by this model.

The successes and shortcomings of the magnetic dipole emission model of pulsars are reviewed and a modification of the model presented. A power-law relation is found statistically between the modifying factor and the time derivative of the period. The decay time scale of the modified field is greater than 108 yr, consistent with the theoretical results. The P ∼ P relation given by the modified model is P ∞ P−3, which is just the observed gradient in the empirical P ∼ P plot above the spinning-up line.

The relation between the radiating cone aperture ϱ and the period P can be more precisely determined if use is made of a correlation between P and a previously defined parameter K. The latter can be calculated from observed beam width and range of variation of the polarization angle. Values of ϱ and the magnetic inclination α estimated by this means are given.

Mean pulse total intensity and polarization data at 1560 MHz are presented for 45 southern pulsars. The observations were made during 1988 at Parkes using a filter-bank polarimeter system. The results are discussed in terms of the rotating vector model for pulse polarization. Notable results include a highly polarized interpulse pulsar and several pulsars with very wide mean pulse profiles

Statistical analysis has been carried out of the relations between period and the ageP−t c, and the inclination of magnetic to rotation axis to the age α−t cof pulsars have been done. Up to characteristic agest c=3×107 years the period increases as expected for magneto-dipole radiation energy lossesP=P m (1−exp(−t/τ B ))1/n−1. Best-fitting parameters of this approximation are the time-scale of the magnetic moment decay τ B =4×106 years and breaking indexn=3.6. Fort c>3×107 years theP−t cdependence is significantly different. The inclination α of magnetic to rotation axis decreases versus age, showing a secular alignment of the axis. But this decrease continues also only up tot c=3×107 years. Thus bothP−t cand α−t cdependencies indicate that most of the pulsars of agest c>3×107 years are not evolutionary continuations of more younger ones, but apparently represent another population of pulsars, which differ by their genetic history or physical processes. This population includes all known millisecond pulsars. We suggest, that this population is a so-called ‘recycled’ pulsar. The list of candidates of ‘recycled’ pulsars is presented. A new evaluation of the inclination of the magnetic to the rotation axis for 105 pulsars is presented.

The effects of aberration, retardation and magnetic field sweep back, which are caused directly or indirectly by pulsar's rapid rotation, are estimated in order to examine their influences on the geometry asymmetry of the mean pulse profile. The geometric asymmetry exhibits different behaviors at different cases. The millisecond pulsars incline to develop mean pulse profiles with asymmetric contrary to the normal pulsars. The pulsar J0437-4715 is analyzed as an example.

We present high-quality observations of PSR B0826-34 at 1374 MHz. The emission from this pulsar exhibits strong bursts of pulses followed by long periods of `null' pulses. When it is strong, the radiation extends through the whole pulse period. We show for the first time that there is weak emission during the `null' phases, which should therefore be considered to be a different mode rather than a null. During this weak mode the profile is similar to that observed in the strong mode at low radio frequency. Using a phase-tracking method, the pattern of drifting subpulses during the strong mode is seen to be coherent across the whole profile. The drift rate is variable and includes positive and negative values. Thirteen subpulse bands have been directly observed, covering the whole longitude range. The subpulses and their spacings ($P_2$) are wider in one half of the profile than those in the other half. This difference, and the variation of observed $P_2$ within the two regions, can be accounted for if the magnetic pole is inclined to the rotation axis by about 0.5 degrees. These two regions appear to represent radiation from outer and inner cones. The intensity modulation of subpulses in all longitude ranges is related to the magnitude of the drift rate., 8 pages, 10 figures. Accepted for publication in MNRAS

Scintillation of pulsar radio emission provides information about the interstellar medium along the path to the pulsar and the velocities of pulsars. It also affects the precision of pulse timing observations. Using a pulsar timing system developed at the Urumqi Astronomical Observatory25 m telescope, we observed diffractive scintillation dynamic spectra for several strong northern pulsars. This paper introduces the observing system and discusses the observational results.

The pulsar’s observation is being developed using the 25m radio telescope at Urumqi Astronomical Observatory (UAO). A pulsar timing system has been set up. It uses a dual polarization receiver operating at 18cm and a filterbank receiver. Timing properties of about 100 pulsars will be monitored with this system. The single channel system at 92 cm works since 1996 for the program of mean pulse profile and long term variation of intensity about 18 pulsars. The observation of spectrum properties for few strong pulsars at 92cm, 18cm, 13cm, 6cm, and 3.6cm is in progress.

The mean pulse of PSRJ2019+2425 is very wide, which consist of three asymmetric separate pulses. The five components were found via fitting the mean profile with multi-gaussian components. There are relative phase shifts, resulted from spin of pulsar and the different emission altitude of components. With very short period and small magnetic inclination angle, the components emitted at outermost place will possibly shift apart from the components at lower altitudes. The two components of outer cone can shift about 180 degree in the longitude, and the shape become very wide and asymmetric.

PSR B2111+46 is studied and analyzed by the method of Gaussian fit separation of the average profile (GFSAP). It has been observed at six frequencies, 408, 610, 925, 1408, 1640, and 4850 MHz, serving as an excellent sample for a multifrequency analysis. Applying the GFSAP method we find that PSR B2111+46 has five components in its profile at all six frequencies. The result supports Rankin’s “core-double cone” model in emission region. On the basis of component decomposition, we discuss the geometrical structure of core, inner cone and outer cone, the emission beam radius, the emission region altitude and the geometry symmetry. We also examine the spectrum characteristics of core, inner cone and outer cone. It is found that the spectrum of the core is steeper than the inner and outer cone.