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Journal articles on the topic 'Pulsar: generale'

Author: Grafiati

Published: 9 March 2023

Last updated: 31 July 2025

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1

Stairs, I. H. "Binary pulsars and tests of general relativity." Proceedings of the International Astronomical Union 5, S261 (2009): 218–27. http://dx.doi.org/10.1017/s1743921309990433.

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AbstractBinary pulsars are a valuable laboratory for gravitational experiments. Double-neutron-star systems such as the double pulsar provide the most stringent tests of strong-field gravity available to date, while pulsars with white-dwarf companions constrain departures from general relativity based on the difference in gravitational binding energies in the two stars. Future observations may open up entirely new tests of the predictions of general relativity.

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2

Desvignes, Gregory, Michael Kramer, Kejia Lee, et al. "Radio emission from a pulsar’s magnetic pole revealed by general relativity." Science 365, no. 6457 (2019): 1013–17. http://dx.doi.org/10.1126/science.aav7272.

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Binary pulsars are affected by general relativity (GR), causing the spin axis of each pulsar to precess. We present polarimetric radio observations of the pulsar PSR J1906+0746 that demonstrate the validity of the geometrical model of pulsar polarization. We reconstruct the (sky-projected) polarization emission map over the pulsar’s magnetic pole and predict the disappearance of the detectable emission by 2028. Two tests of GR are performed using this system, including the spin precession for strongly self-gravitating bodies. We constrain the relativistic treatment of the pulsar polarization m

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3

Chen, Qiang, Yong Zhao, and Lixia Yan. "X-ray Pulsar Signal Denoising Based on Variational Mode Decomposition." Entropy 23, no. 9 (2021): 1181. http://dx.doi.org/10.3390/e23091181.

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Pulsars, especially X-ray pulsars detectable for small-size detectors, are highly accurate natural clocks suggesting potential applications such as interplanetary navigation control. Due to various complex cosmic background noise, the original pulsar signals, namely photon sequences, observed by detectors have low signal-to-noise ratios (SNRs) that obstruct the practical uses. This paper presents the pulsar denoising strategy developed based on the variational mode decomposition (VMD) approach. It is actually the initial work of our interplanetary navigation control research. The original puls

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4

Liang, Ruixing. "Contribution of Pulsars to the AMS-02 Positron Excess." Journal of Physics: Conference Series 2346, no. 1 (2022): 012008. http://dx.doi.org/10.1088/1742-6596/2346/1/012008.

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Abstract In this paper we tested the pulsar interpretation of positron excess, measured by the Alpha Magnetic Spectrometer-02 (AMS-02), by using the list of objects from the Australian National Telescope Facility pulsar catalog (ATNF catalog). We take into account in the calculation the energy losses that cosmic rays encounter when propagating through the Galaxy and we included the secondary positrons which are produced through the collision of cosmic rays against the atoms of the interstellar space. We firstly hypothesized the possibility of a single pulsar contributing to the positron flux.

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5

Malov, IF. "Two Types of Pulsar." Australian Journal of Physics 40, no. 6 (1987): 731. http://dx.doi.org/10.1071/ph870731.

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Some arguments for the subdivision of pulsars into two classes are considered: (i) short-period pulsars described by Smith's (1973) model and (ii) long-period pulsars for which the hollow-cone model is valid. The data for PSR 1937 + 21 (P = 1�56 ms) are in good agreement with this conception, this pulsar being a typical representative of the first group of pulsars.

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6

Ulyanov, O. M. "HISTORY OF LOW-FREQUENCY RESEARCH OF PULSARS." Radio physics and radio astronomy 26, no. 2 (2021): 130–47. http://dx.doi.org/10.15407/rpra26.02.130.

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Purpose: The main most pronounced events, which occurred in the initial period of the pulsars’ study at the decameter wavelength range, are presented. The example of the main scientific problems, which were formulated at the very beginning of pulsar research, shows how the emphasis and priorities of these studies have been changing over time, which tasks have finally been solved, and which are still waiting to be solved. It is shown how the ongoing modernization of the UTR-2 radio telescope have allowed to acquire new qualities in astrophysical research being made with this radio telescope and

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7

Zhou, Shiqi, Erbil Gügercinoğlu, Jianping Yuan, Mingyu Ge, and Cong Yu. "Pulsar Glitches: A Review." Universe 8, no. 12 (2022): 641. http://dx.doi.org/10.3390/universe8120641.

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∼6% of all known pulsars have been observed to exhibit sudden spin-up events, known as glitches. For more than fifty years, these phenomena have played an important role in helping to understand pulsar (astro)physics. Based on the review of pulsar glitches search method, the progress made in observations in recent years is summarized, including the achievements obtained by Chinese telescopes. Glitching pulsars demonstrate great diversity of behaviours, which can be broadly classified into four categories: normal glitches, slow glitches, glitches with delayed spin-ups, and anti-glitches. The ma

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8

Slee, OB, SK Alurkar, and AD Bobra. "Flux Densities, Spectra and Variability of Pulsars at Metre Wavelengths." Australian Journal of Physics 39, no. 1 (1986): 103. http://dx.doi.org/10.1071/ph860103.

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We present the results of two-frequency flux density measurements of 74 pulsars with the Culgoora circular array. We show that the spectral index of a typical pulsar steepens markedly from 80 to 1400 MHz, but we found no significant relationship between the metre-wave spectral index and the published pulsar parameters

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9

Ma, Zhi, Zi-Yi You, Ying Liu, et al. "A Preliminary Study of Large Scale Pulsar Candidate Sifting Based on Parallel Hybrid Clustering." Universe 8, no. 9 (2022): 461. http://dx.doi.org/10.3390/universe8090461.

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Pulsar candidate sifting is an essential part of pulsar analysis pipelines for discovering new pulsars. To solve the problem of data mining of a large number of pulsar data using a Five-hundred-meter Aperture Spherical radio Telescope (FAST), a parallel pulsar candidate sifting algorithm based on semi-supervised clustering is proposed, which adopts a hybrid clustering scheme based on density hierarchy and the partition method, combined with a Spark-based parallel model and a sliding window-based partition strategy. Experiments on the two datasets, HTRU (The High Time-Resolution Universe Survey

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10

Malov, I. F., and O. I. Malov. "On the Evolution of Angles between the Magnetic Moment and the Axis of Rotation in Radio Pulsars." Астрономический журнал 100, no. 2 (2023): 206–18. http://dx.doi.org/10.31857/s0004629923020068.

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Three methods were used to calculate the angles β between the magnetic moment and the axis of rotation of central neutron stars for 307 known radio pulsars. There is no explicit statistical dependence of the calculated angles β on the kinematic age of pulsars. It follows from this that either the indicated angle does not change noticeably with the age of the pulsar, or pulsars are born with an arbitrary inclination angle.

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11

Andharmule, Saransh, Mayank Jain Banda Mutha, and Siya Kothari. "Review of LOFAR and its application on Pulsars." Journal of Physics: Conference Series 2571, no. 1 (2023): 012037. http://dx.doi.org/10.1088/1742-6596/2571/1/012037.

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Abstract Pulsars are magnetized neutron stars which have provided us a great insight into the evolution of the neutron stars themselves. We here present the application of the existing LOFAR technology on Pulsar observation, since LOFAR observes the unexplored frequencies of 10-240 MHz. This paper summarizes the system design of LOFAR and shows how this can be used to observe the Pulsars, since recent studies have presented that pulsars observation is possible in the low frequency range.

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12

Butsaracom, Kritaporn, Brandon Khan Cantlay, and Maneenate Wechakama. "Fitting electron spectrum from AMS-02 by pulsar electrons." Journal of Physics: Conference Series 2145, no. 1 (2021): 012003. http://dx.doi.org/10.1088/1742-6596/2145/1/012003.

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Abstract In this work, we aim to explain the latest data of cosmic-ray electrons from AMS-02 by an electron background model and pulsar electrons. We consider an electron background model which includes primary and secondary electrons. We assume that pulsars are major sources of the electron excess. Since electrons easily lose their energy through the interstellar radiation field and the magnetic field via inverse Compton scattering and synchrotron radiation, respectively, they propagate in a short length. We adopt nearby pulsar data in the distance of 1 kpc from the Australia Telescope Nation

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13

Zhu, Xu, Hui Liu, Xinji Wu, et al. "Statistical Study on the Q Parameter Based on Parkes Data." Universe 10, no. 4 (2024): 175. http://dx.doi.org/10.3390/universe10040175.

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Using the rotating vector model (RVM) and aiming to constrain the value of the magnetic inclination angle (α), we perform a least-squares fit on the linearly polarized position angles of 125 pulsars from Parkes 64 m archive data at 1400 MHz. Subsequently, a statistical analysis of the normalized Q parameters is carried out. Furthermore, based on the Q-parameter, we provide a further understanding of the geometry of the radio emission region of the pulsar. In this statistical sample, about 1/5 of the sample is clustered at 0, suggesting that this part of the pulsar is viewed from the center of

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14

Lazarov, Andon D. "ISAR Imaging of a Rotating Asteroid Irradiated by Pulsar’s Electromagnetic Emission." Cybernetics and Information Technologies 19, no. 2 (2019): 38–50. http://dx.doi.org/10.2478/cait-2019-0014.

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Abstract The aim of the present study is imaging of moving objects, asteroids illuminated by continuous coherent wideband pulsar’s signals. As pulsars are located on more than thousands of light years from Earth, objects crossing pulsars’ emission beams are considered as second sources of electromagnetic waves, carrying object’s shape and velocity information that can be extracted by application pulsar emission-based inverse aperture synthesis. Inverse Synthetic Aperture Radar (ISAR) scenario, geometry and kinematics are analytically described. Models of pulsar signals and ISAR signals seconda

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15

Olmi, Barbara. "Evolved Pulsar Wind Nebulae." Universe 9, no. 9 (2023): 402. http://dx.doi.org/10.3390/universe9090402.

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Based on the expected population of core collapse supernova remnants and the huge number of detected pulsars in the Galaxy, still representing only a fraction of the real population, pulsar wind nebulae are likely to constitute one of the largest classes of extended Galactic sources in many energy bands. For simple evolutionary reasons, the majority of the population is made of evolved systems, whose detection and identification are complicated by their reduced luminosity, the possible lack of X-ray emission (that fades progressively away with the age of the pulsar), and by their modified morp

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16

Stappers, B. W., E. F. Keane, M. Kramer, A. Possenti, and I. H. Stairs. "The prospects of pulsar timing with new-generation radio telescopes and the Square Kilometre Array." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 376, no. 2120 (2018): 20170293. http://dx.doi.org/10.1098/rsta.2017.0293.

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Pulsars are highly magnetized and rapidly rotating neutron stars. As they spin, the lighthouse-like beam of radio emission from their magnetic poles sweeps across the Earth with a regularity approaching that of the most precise clocks known. This precision combined with the extreme environments in which they are found, often in compact orbits with other neutron stars and white dwarfs, makes them excellent tools for studying gravity. Present and near-future pulsar surveys, especially those using the new generation of telescopes, will find more extreme binary systems and pulsars that are more pr

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17

Venkatesh, T. S. Sachin, and Gaurav Pundir. "PERISTOLE: Package That Generates Time Delay Plots Caused by Gravitational Lensing." Research Notes of the AAS 6, no. 12 (2022): 255. http://dx.doi.org/10.3847/2515-5172/aca6ec.

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Abstract We present PERISTOLE to study the various time delays associated with the pulsar rotation and other general relativistic aspects of binary pulsars. It is made available as an open-source python package which takes some parameters of the double pulsar system as input and outputs the rotational and latitudinal lensing delays along with the geometric and Shapiro delays that arise due to gravitational lensing. This package was intended to provide a way to quickly analyze, evaluate and study the differences between variations of the same systems and also to quantify the consequences that d

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18

Malov, I. F., and O. I. Malov. "Analysis of the Parameters of Radio Pulsars with Giant Pulses Using the Principal Component Analysis." Астрономический журнал 100, no. 3 (2023): 272–80. http://dx.doi.org/10.31857/s0004629923030052.

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Clustering of radio pulsars with observable giant pulses (GPs) has been carried out using the principal component analysis. Five parameters were used (period, its derivative, observed luminosity, kinematic age, and the angle between the rotation axis and the magnetic moment of the central neutron star). It was shown that the set of all known GP pulsars is divided into two clusters in the phase space of the principal components. One of the clusters contains four pulsars with short periods and high luminosity; the second cluster contains nine long-period and fainter sources. A separate object, n

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19

Maiorano, Michele, Francesco De Paolis, and Achille A. Nucita. "Principles of Gravitational-Wave Detection with Pulsar Timing Arrays." Symmetry 13, no. 12 (2021): 2418. http://dx.doi.org/10.3390/sym13122418.

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Pulsar timing uses the highly stable pulsar spin period to investigate many astrophysical topics. In particular, pulsar timing arrays make use of a set of extremely well-timed pulsars and their time correlations as a challenging detector of gravitational waves. It turns out that pulsar timing arrays are particularly sensitive to ultra-low-frequency gravitational waves, which makes them complementary to other gravitational-wave detectors. Here, we summarize the basics, focusing especially on supermassive black-hole binaries and cosmic strings, which have the potential to form a stochastic gravi

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Maiorano, Michele, Francesco De Paolis, and Achille A. Nucita. "Description and Application of the Surfing Effect." Universe 8, no. 12 (2022): 620. http://dx.doi.org/10.3390/universe8120620.

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The standard technique for very low-frequency gravitational wave detection is mainly based on searching for a specific spatial correlation in the variation of the times of arrival of the radio pulses emitted by millisecond pulsars with respect to a timing model. This spatial correlation, which in the case of the gravitational wave background must have the form described by the Hellings and Downs function, has not yet been observed. Therefore, despite the numerous hints of a common red noise in the timing residuals of many millisecond pulsars compatible with that expected for the gravitational

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21

Zhou, Linyong, Shanping You, Bimo Ren, Xuhong Yu, and Xiaoyao Xie. "A novel image classification model based on adversarial training for pulsar candidate identification." Journal of Intelligent & Fuzzy Systems 39, no. 5 (2020): 7657–69. http://dx.doi.org/10.3233/jifs-200925.

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Pulsars are highly magnetized, rotating neutron stars with small volume and high density. The discovery of pulsars is of great significance in the fields of physics and astronomy. With the development of artificial intelligent, image recognition models based on deep learning are increasingly utilized for pulsar candidate identification. However, pulsar candidate datasets are characterized by unbalance and lack of positive samples, which has contributed the traditional methods to fall into poor performance and model bias. To this end, a general image recognition model based on adversarial train

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22

Orusa, Luca, Silvia Manconi, Fiorenza Donato, and Mattia Di Mauro. "Constraining positron emission from pulsar populations with AMS-02 data." Journal of Physics: Conference Series 2156, no. 1 (2021): 012086. http://dx.doi.org/10.1088/1742-6596/2156/1/012086.

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Abstract The cosmic-ray flux of positrons is measured with high precision by the space-borne particle spectrometer AMS-02. The hypothesis that pulsar wind nebulae (PWNe) can significantly contribute to the excess of the positron (e+) cosmic-ray flux has been consolidated after the observation of a γ-ray emission at TeV energies of a few degree size around Geminga and Monogem PWNe. In this work we undertake massive simulations of galactic pulsars populations, adopting different distributions for their position in the Galaxy, intrinsic physical properties, pair emission models, in order to overc

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23

Dado, Shlomo, Arnon Dar, Shlomo Dado, and Arnon Dar. "Are fast radio bursts produced by large glitches of anomalous x-ray pulsars?" Physics & Astronomy International Journal 7, no. 1 (2023): 1–5. http://dx.doi.org/10.15406/paij.2023.07.00276.

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Phase transitions within anomalous X-ray pulsars (AXPs) and soft γ-ray repeaters (SGRs) can lead to mini contractions. Such contractions produce pulsar gliches and shock break outs from their surface accompanied by thermal X/γ -ray emission. Highly relativistic dipolar e+e− bunches launched from the pulsar polar caps emit fast radio bursts (FRBs) of narrowly beamed coherent curvature radiation, visible from cosmic distances if they point in the direction of Earth. Although the associated bursts of surface X/γ -rays are nearly isotropic, and many orders of magnitude more energetic than the FRBs

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24

Wu, Kinwah. "Multi-Messenger Astrophysics of a Millisecond Pulsar Orbiting around a Massive Black Hole." Universe 8, no. 2 (2022): 78. http://dx.doi.org/10.3390/universe8020078.

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Extreme-mass-ratio and intermediate-mass-ratio binaries with a millisecond pulsar are gravitational-wave sources that emit also electromagnetic radiation. The millisecond pulsars in these binaries have complex orbital and spin dynamics, which are observable because of spin–orbit and spin–spin coupling (through spin–curvature interaction). The strengths of the couplings generally depends on the mass ratio between the pulsar and the black hole. The narrow mass range of neutron stars gives an advantage in parameter extraction as it greatly reduces the search space, in particular, in the determina

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Kim, Vitaliy, Adel Umirbayeva, and Yerlan Aimuratov. "Estimates of the Surface Magnetic Field Strength of Radio Pulsars." Universe 9, no. 7 (2023): 334. http://dx.doi.org/10.3390/universe9070334.

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We investigate the geometry of the magnetic field of rotation-powered pulsars. A new method for calculating an angle (β) between the spin and magnetic dipole axes of a neutron star (NS) in the ejector stage is considered within the frame of the magnetic dipole energy loss mechanism. We estimate the surface magnetic field strength (Bns) for a population of known neutron stars in the radio pulsar (ejector) stage. The evaluated Bns(β) may differ by an order of magnitude from the values without considering the angle β. It is shown that Bns(β) lies in the range 108–1014G for a known population of s

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26

D’Onofrio, Luca. "The targeted search for gravitational waves from known pulsars." Journal of Physics: Conference Series 2429, no. 1 (2023): 012038. http://dx.doi.org/10.1088/1742-6596/2429/1/012038.

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Abstract In this paper, I review the latest results by the LIGO-Virgo-Kagra Collaboration for the targeted search of continuous gravitational waves (CWs) from 236 pulsars. First, I present an overview of the types of the CW search. Then, I show the results obtained using data from the third observing run of LIGO and Virgo detectors combined with data from the second observing run. No evidence of gravitational waves has been found but it is possible to set upper limits on the CW amplitude and on the pulsar ellipticity at 95% confidence level. 23 of the analyzed pulsars have strain amplitudes th

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27

Xia, Hongbo. "Origin of the Positron Excess with Pulsar Wind Nebulae." Journal of Physics: Conference Series 2386, no. 1 (2022): 012075. http://dx.doi.org/10.1088/1742-6596/2386/1/012075.

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Abstract AMS-02 has been measured with unprecedented precision data for the positron flux. These data show that there is an excess of cosmic positrons detected for energies above 10 GeV with respect to the well known secondary production which is due to the collision of cosmic rays with the atoms of the interstellar medium. In this paper we have investigated the possibility that the positron excess is due to the acceleration of positrons and electrons from pulsar wind nebulae. We have first made the assumption that only one pulsar, Geminga, dominates the production of positrons detected at Ear

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28

Barsukov, D. P., I. K. Morozov, and A. N. Popov. "Influence of a Small-Scale Magnetic Field on the Heating of the Polar Cap of the Radio Pulsar J0901–4046." Письма в Астрономический журнал: Астрономия и космическая астрофизика 49, no. 12 (2023): 869–74. http://dx.doi.org/10.31857/s032001082312001x.

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The pulsar J0901–4046 has a spin periodP = 75.8 s and is themost slowly rotating one amongthe isolated radio pulsars. We have considered the influence of a small-scale magnetic field in the offcentereddipole model on the polar cap heating by the reverse positron current in the inner gap of the pulsar.We have assumed that the electron–positron pairs in the gap are created in bound states, which then arebroken by thermal photons from the stellar surface.

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29

Kazbegi, AZ, GZ Machabeli, and G. Melikidze. "Radio Emission Model of a 'Typical' Pulsar." Australian Journal of Physics 40, no. 6 (1987): 755. http://dx.doi.org/10.1071/ph870755.

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The generation of radio waves in the plasma of the pulsar magnetosphere is considered taking into account the inhomogeneity of the dipole magnetic field. It is shown that the growth rate of the instability of the electromagnetic waves calculated in the non-resonance case turns out to be of the order of 1/ TO (where TO is the time of plasma escape from the light cylinder). However, the generation of electromagnetic waves from a new type Cherenkov resonance is possible, occurring when the particles have transverse velocities caused by the drift due to the inhomogeneity of the magnetic field. Est

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30

Hu, Huanchen, and Paulo C. C. Freire. "Measuring the Lense–Thirring Precession and the Neutron Star Moment of Inertia with Pulsars." Universe 10, no. 4 (2024): 160. http://dx.doi.org/10.3390/universe10040160.

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Neutron stars (NSs) are compact objects that host the densest forms of matter in the observable universe, providing unique opportunities to study the behaviour of matter at extreme densities. While precision measurements of NS masses through pulsar timing have imposed effective constraints on the equation of state (EoS) of dense matter, accurately determining the radius or moment of inertia (MoI) of an NS remains a major challenge. This article presents a detailed review on measuring the Lense–Thirring (LT) precession effect in the orbit of binary pulsars, which would give access to the MoI of

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31

Barnaföldi, Gergely G., Péter Pósfay, Balázs E. Szigeti, and Antal Jakovác. "Estimating compressibility from maximal-mass compact star observations." European Physical Journal Special Topics 229, no. 22-23 (2020): 3605–14. http://dx.doi.org/10.1140/epjst/e2020-000108-4.

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AbstractWe investigated recent observation data of pulsar masses of PSR J0740+6620, PSR J0348+0432, and PSR J1614−2230 based on the extended σ-ω model. We assumed that these pulsars are maximal mass compact star, which suggest that the core approximation can be applied. Using the linear relations between the microscopic and macroscopic parameters of neutron stars suggested by this model, we estimated the values of the nucleon Landau mass and nuclear compressibility mL=776.0−84.9+38.5 MeV and K=242.7−28.0+57.2 MeV, respectively.

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Szigeti, Balázs Endre, Gergely Gábor Barnaföldi, Péter Pósfay, and Antal Jakovác. "Estimating Microscopic Nuclear Data by Compact Star Observations." EPJ Web of Conferences 259 (2022): 13011. http://dx.doi.org/10.1051/epjconf/202225913011.

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We studied recent observation data of pulsar masses and radii of PSR J0740+6620, PSR J0348+0432, and PSR J1614–2230 from different measurements, based on the extended version of σ-ω model. Throughout our analysis, we assumed that these pulsars are maximal-mass compact stars, thus we applied the core approximation. Based on the linear relation between the microscopic and macroscopic parameters of compact stars evaluated by our model, we estimated the average Landau mass mL = 752.46- 42.5+ 49.1 MeV and compressibility K = 261.7- 28.0+ 57.2 MeV.

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Pétri, J. "General-relativistic pulsar magnetospheric emission." Monthly Notices of the Royal Astronomical Society 477, no. 1 (2018): 1035–64. http://dx.doi.org/10.1093/mnras/sty620.

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34

Smith, Keith T. "General relativity reveals pulsar beams." Science 365, no. 6457 (2019): 995.4–996. http://dx.doi.org/10.1126/science.365.6457.995-d.

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35

Backer, D. C., and R. W. Hellings. "Pulsar Timing and General Relativity." Annual Review of Astronomy and Astrophysics 24, no. 1 (1986): 537–75. http://dx.doi.org/10.1146/annurev.aa.24.090186.002541.

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36

Venter, C. "Recent Very-high-energy Results on Pulsars and Pulsar Wind Nebulae." Acta Physica Polonica B Proceedings Supplement 15, no. 3 (2022): 1. http://dx.doi.org/10.5506/aphyspolbsupp.15.3-a9.

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Samodurov, V. A., S. A. Tyul’bashev, M. O. Toropov, A. V. Dolgushev, V. V. Oreshko, and S. V. Logvinenko. "Detection of Two New RRATs at 111 MHz." Астрономический журнал 100, no. 6 (2023): 517–23. http://dx.doi.org/10.31857/s0004629923070071.

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At the LPA LPI radio telescope, a search was conducted for pulse signals in a specific area with declinations +52°δ+55°. The processing involved ten months of observations recorded in six frequency channels, each with a channel width of 415 kHz and a total bandwidth of 2.5 MHz. The analysis of the data revealed 22 000 events, exhibiting a pronounced dispersion delay of signals over the frequency channels, which are indicative of pulsar pulses. These pulses were found to belong to four known pulsars and two new rotating radio transients (RRAT). Additional pulse search was carried out in 32-chan

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38

Milano, L., E. Calloni, R. De Rosa, M. De Laurentis, L. Di Fiore, and F. Garufi. "THE PAST AND THE FUTURE OF DIRECT SEARCH OF GW FROM PULSARS IN THE ERA OF GW ANTENNAS." Acta Polytechnica 53, A (2013): 742–45. http://dx.doi.org/10.14311/ap.2013.53.0742.

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In this paper we will give an overview of the past and present status of Gravitational Wave (GW) research associated with pulsars, taking into account the target sensitivity achieved from interferometric laser GW antennas such as Tama, Geo, Ligo and Virgo. We will see that the upper limits obtained with searches for periodic GW begin to be astrophysically interesting by imposing non-trivial constraints on the structure and evolution of the neutron stars. We will give prospects for the future detection of pulsar GW signals, with Advanced Ligo and Advanced Virgo and future enhanced detectors, e.

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Kimpson, Tom, Kinwah Wu, and Silvia Zane. "Orbital spin dynamics of a millisecond pulsar around a massive BH with a general mass quadrupole." Monthly Notices of the Royal Astronomical Society 497, no. 4 (2020): 5421–31. http://dx.doi.org/10.1093/mnras/staa2103.

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ABSTRACT We investigate the spin dynamics of a millisecond pulsar (MSP) in compact orbit around a Kerr-like massive BH with an general mass quadrupole. We use the Mathisson–Papetrou–Dixon formulation to compute the orbital and spin evolution of the MSP, accounting for the non-linear interaction of the pulsar’s energy–momentum tensor on the background space–time metric. We investigate how the MSP spin and BH quadrupole moment manifest in the pulsar spin-orbital dynamics. We discuss the astrophysical observational implications of these spin and orbital dynamics on the timing of a radio pulsar in

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Melrose, D. B. "Twinkle, Twinkle Little Pulsar/Quasar." Australian Journal of Physics 52, no. 1 (1999): 1. http://dx.doi.org/10.1071/p98076.

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The twinkling of stars is a familiar example of scintillations, due to turbulence in the Earth’s atmosphere causing fluctuations in the refractive index of the air along the line of sight. Scintillations lead to time variations in the apparent position of the source, and hence to an angular broadening on integration over an observation time. Scintillations also lead to fluctuations in the intensity of the source. Pointlike astronomical radio sources such as pulsars and (the compact cores of some) quasars scintillate due to fluctuations in the electron density along the line of sight through th

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Petrov, A. E., A. M. Bykov, S. M. Osipov, A. M. Krassilchtchikov, and K. P. Levenfish. "Pulsars with bow shocks: model constraints of the pulsar wind Lorentz factor." Journal of Physics: Conference Series 1038 (June 2018): 012001. http://dx.doi.org/10.1088/1742-6596/1038/1/012001.

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Li, Zhang, K. S. Cheng, and Mei Dong-Cheng. "Cosmic-Ray Positrons Produced by Pulsar Winds from Mature Gamma-Ray Pulsars." Chinese Physics Letters 18, no. 5 (2001): 701–4. http://dx.doi.org/10.1088/0256-307x/18/5/326.

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Kim, H., H. M. Lee, C. H. Lee, and H. K. Lee. "Pulsar magnetospheres: a general relativistic treatment." Monthly Notices of the Royal Astronomical Society 358, no. 3 (2005): 998–1018. http://dx.doi.org/10.1111/j.1365-2966.2005.08839.x.

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Mestel, L. "General Relativistic Electrodynamics and Pulsar Theory." International Astronomical Union Colloquium 160 (1996): 417–20. http://dx.doi.org/10.1017/s0252921100041993.

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AbstractMuslimov &amp; Tsygan (1986, 1990, 1991, 1992) have shown how the dragging of inertial frames modifies the Goldreich-Julian charge density. The consequences are noted for different models of the electron outflow near the neutron star’s surface.

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Pétri, J. "General-relativistic force-free pulsar magnetospheres." Monthly Notices of the Royal Astronomical Society 455, no. 4 (2015): 3779–805. http://dx.doi.org/10.1093/mnras/stv2613.

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Zhang, Fan. "A Magnetospheric Dichotomy for Pulsars with Extreme Inclinations." Universe 7, no. 12 (2021): 455. http://dx.doi.org/10.3390/universe7120455.

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In this work, we expand on a comment by Lyne et al. (2017), that intermittent pulsars tend to congregate near a stripe in the logarithmic period versus period-derivative diagram. Such a stripe represents a small range of polar cap electric potential. Taking into account also the fact (already apparent in their Figure 7, but not explicitly stated there) that high-fraction nulling pulsars also tend to reside within this and an additional stripe, we make the observation that the two stripes further match the “death lines” for double- and single-pole interpulses, associated with nearly orthogonal

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Shatskii, A. A. "General-relativistic curvature of pulsar vortex structure." Astronomy Letters 27, no. 5 (2001): 304–12. http://dx.doi.org/10.1134/1.1368700.

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WILL, CLIFFORD M. "THE CONFRONTATION BETWEEN GENERAL RELATIVITY AND EXPERIMENT: A 1992 UPDATE." International Journal of Modern Physics D 01, no. 01 (1992): 13–68. http://dx.doi.org/10.1142/s0218271892000033.

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The status of experimental tests of general relativity and of theoretical frameworks for analysing them are reviewed. Einstein’s equivalence principle is well supported by experiments such as the Eötvös experiment, tests of special relativity, and the gravitational redshift experiment. Tests of general relativity have reached high precision, including the light deflection, the Shapiro time delay, the perihelion advance of Mercury, and the Nordtvedt effect in lunar motion. Gravitational wave damping has been detected to half a percent using the binary pulsar, and new binary pulsar systems promi

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Denisov, Dmitry M. "Effects of nonlinear electrodynamics in the magnetic field of a pulsar." Canadian Journal of Physics 92, no. 11 (2014): 1453–59. http://dx.doi.org/10.1139/cjp-2014-0087.

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The eikonal method was used to construct differential equations for beams of electromagnetic waves in magnetic and gravitational fields of pulsars, according to the nonlinear electrodynamics of the vacuum. Integrating these equations using successive approximations allows us to find the ray equations and a parametric form of the law of motion for these beams’ electromagnetic pulses. It is shown that the electromagnetic pulse passing through the magnetic field of the pulsar propagates as two normal waves, arriving at the detector along two different rays and spending different amounts of time i

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Konno, K., and Y. Kojima. "General Relativistic Modification of a Pulsar Electromagnetic Field." Progress of Theoretical Physics 104, no. 6 (2000): 1117–27. http://dx.doi.org/10.1143/ptp.104.1117.

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