Relevant bibliographies by topics / Pulsars

Academic literature on the topic 'Pulsars'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 August 2024

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Journal articles on the topic "Pulsars"

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Moran, Abigail, Chiara M. F. Mingarelli, Megan Bedell, Deborah Good, and David N. Spergel. "Improving Distances to Binary Millisecond Pulsars with Gaia." Astrophysical Journal 954, no. 1 (August 25, 2023): 89. http://dx.doi.org/10.3847/1538-4357/acec75.

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Abstract Pulsar distances are notoriously difficult to measure, and play an important role in many fundamental physics experiments, such as pulsar timing arrays. Here, we perform a cross-match between International PTA pulsars (IPTA) and Gaia's Data Release 2 (DR2) and Data Release 3 (DR3). We then combine the IPTA pulsar’s parallax with its binary companion’s parallax, found in Gaia, to improve the distance measurement to the binary. We find seven cross-matched IPTA pulsars in Gaia DR2, and when using Gaia DR3 we find six IPTA pulsar cross-matches but with seven Gaia objects. Moving from Gaia DR2 to Gaia DR3, we find that the Gaia parallaxes for the successfully cross-matched pulsars improved by 53%, and pulsar distances improved by 29%. Finally, we find that binary companions with a <3.0σ detection are unreliable associations, setting a high bar for successful cross-matches.
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Nice, David J., and Stephen E. Thorsett. "Rotational and Orbital Fluctuations of Eclipsing Binary Pulsar PSR B1744-24A." International Astronomical Union Colloquium 160 (1996): 523–24. http://dx.doi.org/10.1017/s0252921100042275.

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Eclipsing binary pulsars systems highlight an important stage in the evolution of isolated millisecond pulsars. In these systems, the pulsar’s companion is losing mass due to Roche lobe overflow and/or a stellar wind induced by intercepted energy from the pulsar flux. Eventual evaporation of the companions could yield isolated millisecond puslars. PSR B1744-24A was the second eclipsing millisecond pulsar to be discovered (Lyneet al. 1990). It is in a 1.8 hr orbit with a ∼ 0.1 M⊙companion. Its eclipses show some variability, and the pulsar is undetectable at about 25% of observing epochs, presumably because it is completely enveloped by the companion’s outflow (Nice &amp; Thorsett 1992).
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Doroshenko, Oleg V., and Sergei M. Kopeikin. "Relativistic effect of gravitational deflection of light in binary pulsars." International Astronomical Union Colloquium 160 (1996): 131. http://dx.doi.org/10.1017/s0252921100041269.

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Timing formula for data processing of observations of binary pulsars that accounts for the relativistic deflection of light in the gravitational field of the pulsar’s companion is presented, and the measurability of this effect along with its variance estimates is discussed. The deflection of the pulsar’s pulse trajectory in the gravitational field of its companion leads to variation in the pulsar’s rotational phase. This variation appears as a narrow sharp growth of the magnitude of the post-fit residuals in the vicinity of the moment of the superior conjunction of the pulsar with its companion. In contrast to the relativistic Shapiro effect, the amplitude of the effect of gravitational deflection of the pulsar radio beam has two peaks with opposite signs, which become sharper as the inclinationiof the pulsar’s orbit approaches to the right angle. The effect under consideration influences the estimation of parameters of the relativistic Shapiro effect in the binary pulsars with nearly edgewise orbits. Its inclusion in the fitting procedure provides a more careful measurement of the sine of the orbital inclinationi, as well as the masses of the pulsar and its companion. This permits an improved testing of alternative theories of gravity in the strong field regime. The effect of the gravitational deflection of light has been numerically investigated for binary pulsars with nearly edgewise orbits. It is shown that the effect is observed in general only when cosi is less than 0.003. This estimate becomes less restrictive as the pulsar’s spin axis approaches the line of sight.
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Dewey, Rachel J., and James M. Cordes. "Monte Carlo Simulations of Radio Pulsars and Their Progenitors." Symposium - International Astronomical Union 125 (1987): 408. http://dx.doi.org/10.1017/s0074180900161030.

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The formation of neutron stars in binary systems is often used to explain the nature of specific radio pulsars and characteristics of the pulsar population as a whole. We have investigated the extent to which such scenarios provide a self-consistent description of the pulsar population. Using a computer simulation, we modeled the evolution of the main sequence stellar population and compared the predicted neutron star population to the observed radio pulsar population, focusing our attention on the pulsar velocity distribution and the incidence of binary pulsars. These characteristics relate very directly to the binary nature of pulsar progenitors, and are not strongly dependent on models of pulsar magentic field and luminosity evolution.The need to reproduce both the high velocities typical of pulsars and the low incidence of binary pulsars strongly constrains the formation of pulsars in binary systems. Unless one assumes that virtually all pulsars originate in close binary systems, the observed velocity distribution cannot result from the disruption of binary systems by symmetric supernova explosions; some additional acceleration process (e.g. asymmetric supernova mass ejection or asymmetries in pulsar radiation) must act during or soon after a pulsar's formation. It is possible to reproduce the velocity distribution by assuming that all pulsars are born in binary systems with initial orbital periods less than about 30 years. However, the predicted incidence of binaries is then too large by more than an order of magnitude, unless one also assumes that the process of mass transfer from the primary to the secondary is almost always non-conservative, or that the minimum mass necessary for a stripped helium core to explode as a supernova is larger (over 4 M⊙) than currently believed. Further analyses of the radio pulsar population, the X-ray binary population and the abundances of elements ejected in supernovae should help determine which of these alternatives is most reasonble. Additional studies of the main sequence stellar population, accounting more accurately for evolutionary and observational selection effects, will reduce the uncertainties in modeling the formation of the neutron star population.It has also been suggested that the observed correlation between pulsar velocities and magnetic moments (see Cordes, these Proceedings) is induced by the differing evolutionary paths by which stars in binary systems form radio pulsars. Our simulation does not reproduce this correlation, and we do not find any paths likely to produce low velocity, low magnetic field neutron stars not in binary systems.We are submitting a full description of our model and results to The Astrophysical Journal.
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Shearer, Andrew, and Eoin O’ Connor. "Optical pulsars and polarimetry." Proceedings of the International Astronomical Union 13, S337 (September 2017): 191–94. http://dx.doi.org/10.1017/s174392131700998x.

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AbstractDespite the early optical detection of the Crab pulsar in 1969, optical pulsars have become the poor cousin of the neutron star family. Only five normal pulsars have been observed to pulse in the optical waveband. A further three magnetars/SGRs have been detected in the optical/near IR. Optical pulsars are intrinsically faint with a first order luminosity, predicted by Pacini, to be proportional to P−10, where P is the pulsar’s period. Consequently they require both large telescopes, generally over-subscribed, and long exposure times, generally difficult to get. However optical observations have the benefit that polarisation and spectral observations are possible compared to X-ray and gamma-ray observations where polarisation measurements are limited. Over the next decade the number of optical pulsars should increase as optical detectors approach 100% quantum efficiency and as we move into the era of extremely large telescopes where limiting fluxes will be 30 to 100 times fainter compared to existing optical telescopes.
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Wang, Ziteng, David L. Kaplan, Rahul Sengar, Emil Lenc, Andrew Zic, Akash Anumarlapudi, B. M. Gaensler, Natasha Hurley-Walker, Tara Murphy, and Yuanming Wang. "Discovery of a Young, Highly Scattered Pulsar PSR J1032-5804 with the Australian Square Kilometre Array Pathfinder." Astrophysical Journal 961, no. 2 (January 24, 2024): 175. http://dx.doi.org/10.3847/1538-4357/ad0fe8.

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Abstract We report the discovery of a young, highly scattered pulsar in a search for highly circularly polarized radio sources as part of the Australian Square Kilometre Array Pathfinder Variables and Slow Transients survey. In follow-up observations with the Parkes radio telescope, Murriyang, we identified PSR J1032−5804 and measured a period of 78.7 ms, a dispersion measure of 819 ± 4 pc cm−3, a rotation measure of −2000 ± 1 rad m−2, and a characteristic age of 34.6 kyr. We found a pulse scattering timescale at 3 GHz of ∼22 ms, implying a timescale at 1 GHz of ∼3845 ms, which is the third most scattered pulsar known and explains its nondetection in previous pulsar surveys. We discuss the identification of a possible pulsar wind nebula and supernova remnant in the pulsar’s local environment by analyzing the pulsar spectral energy distribution and the surrounding extended emission from multiwavelength images. Our result highlights the possibility of identifying extremely scattered pulsars from radio continuum images. Ongoing and future large-scale radio continuum surveys will offer us an unprecedented opportunity to find more extreme pulsars (e.g., highly scattered, highly intermittent, and highly accelerated), which will enhance our understanding of the characteristics of pulsars and the interstellar medium.
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Sett, S., R. P. Breton, C. J. Clark, M. H. Kerkwijk, and D. L. Kaplan. "A search for radio pulsars in five nearby supernova remnants." Astronomy & Astrophysics 647 (March 2021): A183. http://dx.doi.org/10.1051/0004-6361/201936108.

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Context. Most neutron stars are expected to be born in supernovae, but only about half of supernova remnants (SNRs) are associated with a compact object. In many cases, a supernova progenitor may have resulted in a black hole. However, there are several possible reasons why true pulsar-SNR associations may have been missed in previous surveys: The pulsar’s radio beam may not be oriented towards us; the pulsar may be too faint to be detectable; or there may be an offset in the pulsar position caused by a kick. Aims. Our goal is to find new pulsars in SNRs and explore their possible association with the remnant. The search and selection of the remnants presented in this paper was inspired by the non-detection of any X-ray bright compact objects in these remnants when previously studied. Methods. Five SNRs were searched for radio pulsars with the Green Bank Telescope at 820 MHz with multiple pointings to cover the full spatial extent of the remnants. A periodicity search plus an acceleration search up to 500 m s−2 and a single pulse search were performed for each pointing in order to detect potential isolated binary pulsars and single pulses, respectively. Results. No new pulsars were detected in the survey. However, we were able to re-detect a known pulsar, PSR J2047+5029, near SNR G89.0+4.7. We were unable to detect the radio-quiet gamma-ray pulsar PSR J2021+4026, but we do find a flux density limit of 0.08 mJy. Our flux density limits make our survey two to 16 times more sensitive than previous surveys, while also covering the whole spatial extent of the same remnants. Conclusions. We discuss potential explanations for the non-detection of a pulsar in the studied SNRs and conclude that sensitivity is still the most likely factor responsible for the lack of pulsars in some remnants.
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Bondonneau, Louis, Jean-Mathias Grießmeier, Gilles Theureau, and Maciej Serylak. "Low frequency pulsar observations with the international LOFAR station FR606." Proceedings of the International Astronomical Union 13, S337 (September 2017): 313–14. http://dx.doi.org/10.1017/s1743921317009656.

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AbstractThe pulsar’s signal passes through the interstellar medium (ISM) which leads to both chromatic dispersive delays and multipath pulse broadening. These effects have a strong frequency dependence (f−2 and f−4 respectively). Pulse profiles of pulsars are also frequency-dependent leading to some degeneracy with the ISM imprint. Furthermore, many pulsars show a turnover of their spectrum around ~100 MHz. For all these reasons, the frequency band below 100 MHz contains a lot of information about both the pulsar emission and the ISM. Our study is based on a LOw Frequency ARray (LOFAR) monitoring campaign using the international station FR606. Firstly, we demonstrate the importance of a monitoring campaign. Secondly, we calculate median spectra and locate the turnover frequency for 3 pulsars (B0809+74, B1133+16, B1508+55).
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WANG, WEI. "DISTANCE INDICATORS OF GAMMA-RAY PULSARS." International Journal of Modern Physics: Conference Series 23 (January 2013): 289–94. http://dx.doi.org/10.1142/s2010194513011483.

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Distance measurements of gamma-ray pulsars are challenging questions in present pulsar studies. The Large Area Telescope (LAT) aboard the Fermi gamma-ray observatory discovered more than 100 gamma-ray pulsars including 24 new gamma-selected pulsars which nearly have no distance information. We study the relation between gamma-ray emission efficiency (η = Lγ/Ė) and pulsar parameters for young radio-selected gamma-ray pulsars with known distance information in the first gamma-ray pulsar catalog reported by Fermi/LAT. We have introduced three generation order parameters to describe gamma-ray emission properties of pulsars, and find the strong correlation of η – ζ3 a generation order parameter which reflects γ-ray photon generations in pair cascade processes induced by magnetic field absorption in pulsar magnetosphere. A good correlation of η – B LC the magnetic field at the light cylinder radius is also found. These correlations would be the distance indicators in gamma-ray pulsars to evaluate distances for gamma-selected pulsars. Distances of 25 gamma-selected pulsars are estimated, which could be tested by other distance measurement methods. Physical origin of the correlations may be also interesting for pulsar studies.
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Zhang, Xinyuan, Ping Shuai, Liangwei Huang, Shaolong Chen, and Lihong Xu. "Mission Overview and Initial Observation Results of the X-Ray Pulsar Navigation-I Satellite." International Journal of Aerospace Engineering 2017 (2017): 1–7. http://dx.doi.org/10.1155/2017/8561830.

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The newly launched X-ray pulsar navigation-I (XPNAV-1) is an experimental satellite of China that is designed for X-ray pulsar observation. This paper presents the initial observation results and aims to recover the Crab pulsar’s pulse profile to verify the X-ray instrument’s capability of observing pulsars in space. With the grazing-incidence focusing type instrument working at the soft X-ray band (0.5–10 keV), up to 162 segments of observations of the Crab pulsar are fulfilled, and more than 5 million X-ray events are recorded. Arrival times of photons are corrected to the solar system barycentre, and the 33 ms pulse period is sought out for Crab. Epoch folding of all the corrected photon times generates the refined pulse profile of Crab. The characteristic two-peak profile proves that the Crab pulsar has been clearly seen, so that the conclusion is made that XPNAV-1’s goal of being capable of observing pulsars is achieved.
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Dissertations / Theses on the topic "Pulsars"

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Desvignes, Grégory. "L'observation des pulsars au Radiotélescope de Nançay : applications à la recherche de nouveaux objets, à l'étude des systèmes binaires relativistes et à la détection d'un fond d'ondes gravitationnelles." Phd thesis, Université d'Orléans, 2009. http://tel.archives-ouvertes.fr/tel-00496806.

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Un pulsar est une étoile à neutrons en rotation rapide et dotée d'un fort champ magnétique qui peut se manifester en émettant sur tout le spectre électromagnétique. Dans cette thèse, je m'intéresse au rayonnement radio produit par l'étoile. Je commence ainsi par décrire l'instrumentation de dédispersion cohérente à base de GPUs installée au Radiotélescope de Nançay avec deux autres modes d'observation que j'ai développés : un mode pour la recherche de nouveaux pulsar et un mode spectromètre. Une autre partie de ce travail détaille le retraitement en cours du sondage Foster fait à la fin des années 90 à Nançay ainsi que de nouvelles observations ciblées, sur des candidats HESS notamment. Je présente ensuite les résultats obtenus sur les pulsars relativistes J0737-3039A et J1906+0746 avec respectivement des tests de la Relativité Générale et la mesure de la précession géodétique. Des données de polarimétrie ont ainsi permis de déterminer la géométrie du système de PSR J1906+0746. Enfin, je termine par l'analyse des temps d'arrivées de 20 pulsars millisecondes observés à Nançay dans le cadre de l'EPTA, une collaboration européenne pour un réseau de chronométrage pulsar avec pour objectif la détection d'un fond d'ondes gravitationnelles, possible d'ici 5 à 10 ans.
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Livingstone, Margaret Anne. "Timing young pulsars: challenges to standard pulsar spin-down models." Thesis, McGill University, 2010. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=94909.

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Pulsars are rapidly rotating neutron stars which are often noted for their very regular rotation rates. Young pulsars however, frequently exhibit two types of deviations from steady spin down, ``glitches'' - sudden jumps in spin frequency, which provide insight into pulsar interiors, and ``timing noise,'' a smooth stochastic wander of the pulse phase over long time periods. The youngest pulsars also offer a window into the physics that govern pulsar spin down via the measurement of the "braking index'' - a parameter that relates the observable spin frequency of the pulsar with the slowing down torque acting on the neutron star. This thesis discusses long-term timing observations of two young pulsars. First, we present observations of PSR J0205+6449, acquired with the Green Bank Telescope, the Jodrell Bank Observatory and the Rossi X-ray Timing Explorer. We present phase-coherent timing analyses showing timing noise and two spin-up glitches. We also present an X-ray pulse profile analysis showing that the pulsar is detected up to approximately 40 keV and does not vary appreciably over four years. We report the phase offset between the radio and X-ray pulse, showing that the radio pulse leads by 0.10+/-0.01 in phase. We compile measurements of phase offsets for this and other X-ray and gamma-ray pulsars and show that there is no relationship between pulse period and phase offset. Next, we present 10 years of monitoring of PSR J1846-0258 with the Rossi X-ray Timing Explorer. We report the first measurement of the braking index for this pulsar, n=2.65+/-0.01, only the sixth such measurement ever made, and show that the pulsar experienced a small glitch in 2001. In May 2006, PSR J1846-0258 was briefly transformed: it exhibited a series of X-ray bursts, a dramatic increase in the source flux, and significant softening of its X-ray spectrum - behaviours best explained in the context of the magnetar model. PSR J1846-0258 was thus identified as the first rotation-po
Les pulsars, des étoiles à neutrons tournant rapidement sur elles-mêmes, sont reconnus pour leur vitesse de rotation très régulière. Les jeunes pulsars, par contre, présentent fréquemment des comportements qui dévient du ralentissement uniforme de leur vitesse de rotation: des glitchs, variations brutales de la fréquence de révolution qui nous aident à comprendre l'intérieur des plusars, et le bruit chronométrique, une variation stochastique de la phase de rotation sur une longue échelle de temps. Les pulsars les plus jeunes nous offrent aussi un aperçu de la physique qui gouverne le ralentissement de la vitesse de rotation par l'indice de freinage, un paramètre qui relie la fréquence de rotation d'un pulsar au torque qui agit sur lui, et dont la valeur diminue graduellement. Cette thèse discute du chronométrage à long terme de deux jeunes pulsars. Tout d'abord, nous présentons des observations de PSR J0205+6449 acquises avec l'Observatoire de Green Bank, l'Observatoire Jodrell Bank ainsi que le Rossi X-ray Timing Explorer. Nous présentons l'analyse du chronométrage à phase cohérente montrant du bruit chronométrique ainsi que deux glitchs. Nous présentons aussi une analyse du profil du pulse en rayons X montrant que le pulsar est détectable jusqu'à ~40 keV et ne varie pas significativement sur quatre ans. Nous rapportons une mesure de la différence de phase entre le pulse radio et le pulse en rayons X, montrant que le pulse radio précède le pulse en rayons X par 0.10+/-0.01. Une compilation des différences de phase pour ce pulsar et d'autres qui émettent en rayons X et en rayons gamma montre qu'il n'y a aucune relation entre la période de rotation et la différence de phase. Ensuite, nous présentons 10 années de suivi de PSR J1846-0258 avec le Rossi X-ray Timing Explorer. Nous rapportons la première mesure de l'indice de freinage pour ce pulsar, n=2.65+/-0.01, le sixième indice mesuré à ce jour, et montrons que ce pul
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Jacoby, Bryan Anthony Hillenbrand Lynne A. "Recycled pulsars /." Diss., Pasadena, Calif. : California Institute of Technology, 2005. http://resolver.caltech.edu/CaltechETD:etd-01272005-015012.

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Brook, Paul Richard. "The variability of radio pulsars." Thesis, University of Oxford, 2015. http://ora.ox.ac.uk/objects/uuid:65ae413c-cd12-408b-843c-60886cecf1b7.

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Neutron stars are amongst the most exotic objects known in the universe; more than a solar mass of material is squeezed into an object the size of a city, leading to a density comparable to that of an atomic nucleus. They have a surface magnetic field which is typically around a trillion times stronger than the magnetic field here on Earth, and we have observed them to spin up to around 700 times per second. The existence of neutron stars was first proposed by Baade and Zwicky in 1934 but later graduated from theory to fact in 1967 as the first pulses were detected by Jocelyn Bell-Burnell, a then graduate student at the University of Cambridge. There are now well over 2000 neutron stars whose radio emission beams point at, and have been detected on Earth. We call these objects pulsars. Because of their remarkable properties, pulsars are very useful to physicists, who can employ them as precision timing tools due to the unwavering nature of their emission and of their rotation. Having an array of ultra-accurate clocks scattered throughout our galaxy is very useful for performing astrophysical experiments. In particular, precise pulsar timing measurements and the models that explain them, will permit the direct detection of gravitational radiation; a stochastic background initially, and potentially the individual signals from supermassive black hole binaries. Our models of pulsar behaviour are so precise that we are now able to notice even slight departures from them; we are starting to see that unmodelled variability in pulsars occurs over a broad range of timescales, both in emission and in rotation. Any unmodelled variability is, of course, detrimental to the pulsar's utility as a precision timing tool, and presents a problem when looking for the faint effects of a passing gravitational wave. We are hoping that pulsar timing arrays will detect gravitational radiation in the coming decade, but this depends, in part, on our ability to understand and mitigate the effects of the unmodelled intrinsic instabilities that we are observing. One important clue as to the nature of the variability in pulsar emission and rotation, is the emerging relationship between the two; we sometimes observe correlation on timescales of months and years. We have been observing pulsars for almost fifty years and our expanding datasets now document decades of pulsar behaviour. This gives us the ability to investigate pulsar variability on a range of timescales and to gain an insight into the physical processes that govern these enigmatic objects. In this thesis I describe new techniques to detect and analyse the emission and rotational variability of radio pulsars. We have employed these techniques on a 24 year pulsar dataset to unearth a striking new example of a dramatic and simultaneous shift in a pulsar's emission and rotation. We hypothesise that this event was caused by an asteroid interaction, although other explanations are also possible. Our variability techniques have also been used to analyse data from 168 young, energetic pulsars. In this thesis we present results from the nine most interesting. Of these, we have found some level of correlated variability in seven, one of which displays it very strongly. We have also assessed the emission stability of the NANOGrav millisecond pulsars and have found differing degrees of variability, due to both instrumental and astrophysical causes. Finally, we propose a method of probing the relationship between emission and rotation on short-timescales and, using a simulation, we have shown the conditions under which this is possible. Throughout the work, we address the variability in pulsar emission, rotation and links between the two, with the aim of improving pulsar timing, attaining a consolidated understanding of the diverse variable phenomena observed and elucidating the evolutionary path taken by pulsars.
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Yardley, Daniel Roger Billing. "Studying gravitational waves with pulsars : results from the Parkes pulsar timing array." Thesis, The University of Sydney, 2011. https://hdl.handle.net/2123/29163.

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This thesis addresses the problem of gravitational-wave (GW) detection using radio timing observations of pulsars. We study GW signals in real and simulated pulsar timing observations, and describe the astrophysical implications for cases in which no GW signal is detected. We simulate timing observations from a range of hypothetical pulsar timing array projects. The pulse arrival times are then perturbed by an individual source of GWs. One of the simulated data sets comprises an array of 20 pulsars timed with a root-mean-square residual of 10 ns over 10 years. If there is no detectable GW signal in this data set, then the merger rate of supermassive black-hole binaries (SMBHBs) with a chirp mass of 109 solar masses is less than one merger every 105 years up to a redshift of z = 2. This constraint rules out estimates of the SMBHB merger rate based on hierarchical galaxy formation with standard assumptions on the merger parameters. Applying a similar analysis to recently published observations from the Parkes Pulsar Timing Array (PPTA) yields a constraint on the merger rate of SMBHBS of less than one merger every five years for SMBHBs with chirp mass ~ 1010 solar masses up to a redshift of z = 2. The results also indicate that it is unlikely that an individual GW source could be detected with existing data sets. We consider the signal caused by an isotropic stochastic gravitational-wave background (GWB), and show that, with a few more years of observations, either the GWB will be detected or the parameter space of most current galaxy evolution models will be significantly constrained. An analysis of the cross-correlation between the timing residuals of different pulsars in the PPTA shows that there is no detectable GWB signal in the current data. The GWB detection statistic is dominated by only a few pulsars in the current PPTA data. There are good prospects for detection of the GWB using radio timing of pulsars in the next decade. We conclude that the effect of instabilities in realisations of the terrestrial timescale and inaccuracies in the solar system ephemeris must be removed from the timing residuals in order to detect a GW signal in pulsar timing observations in the future. The forthcoming International Pulsar Timing Array project will also significantly increase the probability of detection of GW signals using pulsar timing.
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Octau, Franck. "Exploration d'un grand relevé à Nançay et diversité de la population de pulsars." Thesis, Orléans, 2017. http://www.theses.fr/2017ORLE2042/document.

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Depuis la découverte du premier pulsar en 1967, nous connaissons désormais plus de 2500 pulsars aujourd’hui. Les pulsars offrent un champ d’études considérable : depuis l’étude des propriétés du milieu interstellaire et l’étude de la magnétosphère des pulsars jusqu’aux tests de la gravité en champ fort et la caractérisation d’un fond d’ondes gravitationnelles d’origine cosmologique. Cela explique pourquoi nous continuons de chercher de nouveaux pulsars de nos jours. Après des découvertes de pulsars millisecondes dans les sources non identifiées du Fermi Large Area Telescope, un programme de recherche de nouveaux pulsars a été mené à partir de 2012 par G. Desvignes. Observant à 1.4 GHz avec une haute résolution temporelle et fréquentielle, le programme SPAN512 a été conçu pour la recherche de pulsars rapides et lointains situés dans le plan Galactique. Nous décrirons les méthodes d’analyse mises en place pour traiter les données afin de trouver de nouveaux pulsars, méthodes soit basées sur la stabilité de la période de rotation des pulsars soit sur leur émission d’impulsions individuelles. Nous présenterons aussi l’état actuel de l’analyse du programme SPAN512 et les découvertes effectuées, plus particulièrement du pulsar trouvé au cours de ce travail de thèse, PSR J2055+3829, un pulsar milliseconde de période de rotation de 2.08 ms appartenant à un système de type « Veuve Noire ». Ce sera l’occasion de présenter les études chronométriques réalisées pour trouver l’éphéméride de ce pulsar et, dans le même temps, j’en profiterai pour parler d’une analyse similaire faite sur le pulsar J1618-3921, un pulsar dans une orbite excentrique. Enfin, nous présenterons des études polarimétriques de pulsars réalisées à la lumière d’un nouveau modèle, le modèle du vecteur tournant décentré (DRVM). Nous montrerons qu’un champ magnétique hautement décentré peut expliquer les variations brusques de l’angle de polarisation
Since the discovery of the first pulsar in 1967, we know over 2500 pulsars today. Pulsars offer a broad range of studies: from the study of the properties of interstellar medium and of pulsar magnetospheres up to test of gravity in the strong-field regime and the characterisation of the cosmological Gravitation Waves background. This explains why we keep searching pulsars nowadays. After successful detections of new millisecond pulsars in Fermi Large Area Telescope unassociated sources at Nançay, a blind pulsar survey was initiated in 2012 by G. Desvignes. Conducted at 1.4 GHz with short sampling time and narrow frequency channels, the SPAN512 was designed to find fast and distant pulsars within the Galactic plane. We describe the methods to analyse data in order to find new pulsars, thanks to their spin stability or tto their single pulses. We will also describe the current status of the survey and the discoveries, more especially the pulsar discovered during this thesis, PSR J2055+3829, a 2.08 ms pulsar in a black widow system. It will be the opportunity to present the radio timing analysis of this pulsar and, in the same time, we will describe similar studies conducted on the pulsar J1618-3921, a pulsar in an eccentric orbit. Finally, we present some polarisation studies of pulsars in light of a new model, the Decentred Rotating Vector Model (DRVM). We will show that a highly decentred dipole may explain abrupt variations of polarisation profiles
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Edwards, Russell T. "Pulsar searching /." Australian Digital Theses Program, 2001. http://adt.lib.swin.edu.au/public/adt-VSWT20050323.141044.

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Thesis (Ph.d.) - Swinburne University of Technology, 2001.
Submitted for the degree of Doctor of Philosophy, Swinburne University of Technology, 2001. Typescript. Includes bibliographical references (p. 122-131).
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Icdem, Burcin. "Viscous Time Scale In Accreting Powered Pulsars And Anomalous X-ray Pulsars." Master's thesis, METU, 2011. http://etd.lib.metu.edu.tr/upload/12613373/index.pdf.

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In this thesis we analyse X-ray data of accretion powered low mass and high mass X-ray binaries to understand the nature of their accretion mechanisms by searching for some clues of viscous time-scales of their accretion discs, if they have, in their low frequency power density spectra created from their long-term X-ray observations, or by doing pulse timing analysis with much shorter X-ray data to detect the effects of torque fluctuations caused by the accreting material on the pulsar. The low mass and high mass X-ray binaries we analysed have breaks in their power density spectra, which are attributed to the role of viscosity in the formation of accretion discs. Although, the time-scales corresponding to these break frequencies are smaller than the predictions of the Standard theory of accretion discs, the sources give consistent results among themselves by displaying the expected correlation between their break and orbital frequencies. The correlation curve of LMXBs implies thicker appearing accretion discs than those assumed by the theory. The dichotomy of the HMXBs on this curve points out the different origins of accretion that these sources may have, and offers a way to distinguish the stellar-wind fed systems from the Roche-lobe overflow systems. The timing and spectral analysis of Swift J1626.6-5156 reveal a correlation between the spin-up rate and the luminosity of the source implying that the pulsar is accretion-powered. This correlation together with the characteristics of the X-ray spectra enables us to estimate the magnetic field and the distance of the source. The AXP 1E 2259+586 does not display any signs of viscous time-scale in its low frequency power density spectra, and its pulse timing analysis gives a much smaller torque noise value than that expected from accretion powered pulsars. In addition, the analysis results presented in this thesis reveal magnetar-like glitches which differ than those of radio pulsars, due to the presence of the strong magnetic field of the pulsar. These results eliminate the possibility that the AXP is an accretion-powered pulsar.
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Voûte, Jan Lodewijk Lancelot. "The many shapes of giant pulses radio pulsar research at WSRT /." [S.l. : Amsterdam : s.n.] ; Universiteit van Amsterdam [Host], 2001. http://dare.uva.nl/document/92733.

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Tang, Pui-shan Anisia, and 鄧佩姗. "Thermal X-ray pulses resulting from pulsar glitches." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1999. http://hub.hku.hk/bib/B29790992.

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Books on the topic "Pulsars"

1

Bhattacharyya, Sudip, Alessandro Papitto, and Dipankar Bhattacharya, eds. Millisecond Pulsars. Cham: Springer International Publishing, 2022. http://dx.doi.org/10.1007/978-3-030-85198-9.

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Leeuwen, Joeri van. Radio pulsars. [S.l: s.n.], 2004.

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Albert Gerardus Johannes van Leeuwen. Radio pulsars. [S.l: s.n.], 2004.

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1964-, Phillips J. A., Thorsett Stephen Erik, and Kulkarni S. R. 1956-, eds. Planets around pulsars. San Francisco, Calif: Astronomical Society of the Pacific, 1993.

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Becker, Werner, ed. Neutron Stars and Pulsars. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76965-1.

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A, Prince Thomas, and United States. National Aeronautics and Space Administration., eds. Observations of accreting pulsars. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Morozov, Alexander D. Pulsars: Theory, categories and applications. Hauppauge, N.Y: Nova Science Publishers, 2009.

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Shuai, Ping. Understanding Pulsars and Space Navigations. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-16-1067-7.

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Isaac Asimov. Black holes, pulsars, and quasars. Milwaukee: Gareth Stevens Pub., 2005.

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Isaac Asimov. Quasars, pulsars, and black holes. New York, N.Y: Dell Pub., 1990.

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Book chapters on the topic "Pulsars"

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Verschuur, Gerrit. "Pulsars." In Astronomers' Universe, 101–14. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-13422-2_8.

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Backer, Don C. "Pulsars." In Astronomy and Astrophysics Library, 480–521. New York, NY: Springer New York, 1988. http://dx.doi.org/10.1007/978-1-4612-3936-9_11.

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Courvoisier, Thierry J. L. "Pulsars." In High Energy Astrophysics, 205–24. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-30970-0_14.

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Lang, Kenneth R. "Pulsars." In Astrophysical Data, 605–52. New York, NY: Springer US, 1992. http://dx.doi.org/10.1007/978-1-4684-0640-5_22.

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Mertz, Lawrence. "Pulsars." In Excursions in Astronomical Optics, 109–25. New York, NY: Springer New York, 1996. http://dx.doi.org/10.1007/978-1-4612-2386-3_6.

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Raychaudhuri, A. K., S. Banerji, and A. Banerjee. "Pulsars." In Astronomy and Astrophysics Library, 144–58. New York, NY: Springer New York, 1992. http://dx.doi.org/10.1007/978-1-4612-2754-0_12.

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Carreto Fidalgo, David. "Pulsars and Pulsar Wind Nebulae." In Revealing the Most Energetic Light from Pulsars and Their Nebulae, 19–47. Cham: Springer International Publishing, 2019. http://dx.doi.org/10.1007/978-3-030-24194-0_2.

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Singal, Ashok K. "Giant Radio Pulses from Pulsars." In Sources and Scintillations, 61–64. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-1001-6_11.

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Krolik, J. H. "Millisecond Pulsars." In Highlights of Astronomy, 161–65. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-0977-9_23.

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Beskin, V. S., S. V. Chernov, C. R. Gwinn, and A. A. Tchekhovskoy. "Radio Pulsars." In The Strongest Magnetic Fields in the Universe, 213–43. New York, NY: Springer New York, 2016. http://dx.doi.org/10.1007/978-1-4939-3550-5_7.

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Conference papers on the topic "Pulsars"

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Lomiashvili, D., G. Machabeli, I. Malov, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Drift Wave Model of Part Time Radio Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900113.

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Maan, Yogesh, Avinash A. Deshpande, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Revisiting the rich sub-pulse patterns of B1237+25: Preliminary Results." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900114.

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Mitra, Dipanjan, Joanna M. Rankin, S. Sarala, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Are ‘Partial Cones’ Aberrated Cones?" In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900115.

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Mitra, Dipanjan, Joanna M. Rankin, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "On the Subpulse Modulation and Carousal Circulation Time of PSR B1857–26." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900116.

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Woods, Peter M., C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Observations of Magnetars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900149.

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Rankin, Joanna M., Ben Stappers, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "The Drift Modes of Pulsar B0943+10." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900117.

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Suleymanova, Svetlana A., Joanna M. Rankin, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Emission of Pulsar B0943+10 in the ‘B’urst Mode: Remarkably Continual Changes in the Subpulse Drift Rate and in Integrated Pulse Shape." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900118.

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Bilous, A. V., V. I. Kondratiev, M. V. Popov, V. A. Soglasnov, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Review of overall parameters of giant radio pulses from the Crab pulsar and B1937+21." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900119.

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Kramer, Michael, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Observations of Pulsed Emission from Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900120.

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Karuppusamy, R., B. W. Stappers, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Giant Pulses in Crab and B1133+16." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900121.

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Reports on the topic "Pulsars"

1

Grove, J. E., J. D. Kurfess, B. F. Phlips, M. S. Strickman, and M. P. Ulmer. OSSE Observations of X-Ray Pulsars. Fort Belvoir, VA: Defense Technical Information Center, January 1995. http://dx.doi.org/10.21236/ada464467.

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Strickman, M. S., J. E. Grove, W. N. Johnson, R. L. Kinzer, R. A. Kroeger, J. D. Kurfess, D. A. Grabelsky, et al. OSSE Observations of the Vela and Geminga Pulsars. Fort Belvoir, VA: Defense Technical Information Center, January 1996. http://dx.doi.org/10.21236/ada464424.

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Mahajan, S. M., G. Z. Machabeli, and A. D. Rogava. Escaping radio emission from pulsars: Possible role of velocity shear. Office of Scientific and Technical Information (OSTI), January 1997. http://dx.doi.org/10.2172/468589.

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Gonthier, P. L. Radio-Loud and Radio-Quiet Gamma-Ray Pulsars from the Galactic Plane and the Gould Belt. Office of Scientific and Technical Information (OSTI), March 2005. http://dx.doi.org/10.2172/839940.

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Apte, Zachary. Balloon-Borne Gamma-Ray Polarimeter (PoGO) to Study Black Holes, Pulsars, and AGN Jets: Design and Calibration(SULI). Office of Scientific and Technical Information (OSTI), December 2005. http://dx.doi.org/10.2172/877479.

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Faltens, Andris. Induction Linac Pulsers. Office of Scientific and Technical Information (OSTI), January 2011. http://dx.doi.org/10.2172/1005003.

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Ulmer, M. P., S. M. Matz, R. A. Cameron, D. A. Grabelsky, J. E. Grove, W. N. Johnson, G. V. Jung, et al. OSSE Observations of the Crab Pulsar. Fort Belvoir, VA: Defense Technical Information Center, January 1991. http://dx.doi.org/10.21236/ada461745.

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Strickman, M. S., J. E. Grove, W. N. Johnson, R. L. Kinzer, R. A. Kroeger, J. D. Kurfess, D. A. Grabelsky, S. M. Matz, W. R. Purcell, and M. P. Ulmer. OSSE Observations of the Vela Pulsar. Fort Belvoir, VA: Defense Technical Information Center, January 1993. http://dx.doi.org/10.21236/ada464425.

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Weber, Peter M. Ultrashort Electron Pulses. Fort Belvoir, VA: Defense Technical Information Center, November 1999. http://dx.doi.org/10.21236/ada378937.

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Schroeder, P. C., M. P. Ulmer, S. M. Matz, D. A. Grabelsky, W. R. Purcell, J. E. Grove, W. N. Johnson, et al. OSSE Upper Limits to Pulsar Gamma-Ray Emission. Fort Belvoir, VA: Defense Technical Information Center, September 1994. http://dx.doi.org/10.21236/ada464427.

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