Relevant bibliographies by topics / PULSTAR

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'PULSTAR'

Author: Grafiati
Published: 4 June 2021
Last updated: 8 February 2022

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Journal articles on the topic "PULSTAR"

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Hawari, A. I., S. A. Lassell, and G. I. Gibson. "INTERNET REACTOR LABORATORY: A NUCLEAR REACTOR PHYSICS AND ENGINEERING EDUCATION MODALITY FOR THE 21st CENTURY." EPJ Web of Conferences 247 (2021): 14004. http://dx.doi.org/10.1051/epjconf/202124714004.

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The “second generation” Internet Reactor Laboratory (IRL) has been installed and is currently functional at the PULSTAR reactor of the Nuclear Reactor Program (NRP) at North Carolina State University (NCSU). The NRP has offered IRL based reactor physics experiments and training to external academic institutions and organizations since 2004. In 2016, the United States and the Republic of Vietnam entered into an Administrative Arrangement under Section 123 of the Atomic Energy Act, with a goal of enhancing nuclear training and education for Vietnamese engineering students. Funding was provided by the DOE to upgrade the PULSTAR IRL infrastructure to state-of-the-art remote data acquisition and video teleconferencing capabilities supporting content sharing across multiple remote user platforms. Subsequently, a Cisco Telepresence and LabView reactor data acquisition system were installed and commissioned at the PULSTAR facility. Using this “second generation” system, and during IRL sessions, up to 100 remote students may interact with the control room staff via the Telepresence system using their mobile device or PC, and view 130 channels of live reactor telemetry via the remote client LabView application while recording the data for subsequent review and analysis. LabView graphical user interfaces (GUI) are provided for each IRL module, and incorporate embedded supporting documents such as schematics and diagrams that aid in illustrating associated technical details and concepts. Consequently, the educational experience offered to remote students and trainees is enhanced and assured to be of the same quality as offered to onsite students/trainees at NCSU.
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Mishra, Kaushal K., and Ayman I. Hawari. "Phase contrast neutron imaging at the PULSTAR reactor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 652, no. 1 (October 2011): 615–19. http://dx.doi.org/10.1016/j.nima.2010.09.113.

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Xiao, Ziyu, Kaushal K. Mishra, Ayman I. Hawari, Philip R. Bingham, Hassina Z. Bilheux, and Kenneth W. Tobin. "Coded source neutron imaging at the PULSTAR reactor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 652, no. 1 (October 2011): 606–9. http://dx.doi.org/10.1016/j.nima.2010.10.049.

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Pullela, Sunita V. "Determination of the PULSTAR reactor neutron energy spectrum." Energy Conversion and Management 38, no. 10-13 (July 1997): 1015–23. http://dx.doi.org/10.1016/s0196-8904(96)00131-8.

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Hawari, A. I., M. Liu, and Q. Cai. "FACILITIES FOR NANO MATERIALS EXAMINATION AT THE PULSTAR REACTOR." EPJ Web of Conferences 247 (2021): 08012. http://dx.doi.org/10.1051/epjconf/202124708012.

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The PULSTAR is a 1-MWth nuclear research reactor located at North Carolina State University. It is fueled by uranium dioxide assemblies enriched to 4% or 6% in U-235 and is currently under licensing for operation at 2-MWth power. The PULSTAR is a center for irradiation testing and pre/post irradiation examination of materials. Among its unique capabilities are positron annihilation spectroscopy (PAS) and neutron powder diffraction (NPD) facilities. The PAS facility provides an intense positron beam reaching 6 × 108 e+/s, which drives two spectrometers; the e+-PAS and the Ps-PAS, used for studies of defects in thin film materials. A Na-22 bulk PAS system is also operational, which is used for studying millimeter scale materials. All spectrometers are capable of performing Doppler Broadening Spectroscopy (DBS) and Positron Annihilation Lifetime Spectroscopy (PALS). To date, the PAS systems have been used to characterize various materials (unirradiated and irradiated) that include graphite, soft matter, and metal-organic frameworks (MOF). The NPD facility uses a double focusing single crystal silicon rotating monochromator producing neutron beams with different energies. A position sensitive detection bank covers a scattering angle of 5°-125°. The facility is used in the examination of unirradiated and irradiated materials including graphitic materials, magnetic materials without rare-earth elements, and anode materials used in lithium batteries. The collected diffraction patterns can be processed to produce atomic pair distribution functions. The PAS and NPD facilities are available through user programs including the US DOE’s Nuclear Science User Facilities (NSUF) and the US NSF’s Research Triangle Nanotechnology Network (RTNN).
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Korobkina, E., B. W. Wehring, A. I. Hawari, A. R. Young, P. R. Huffman, R. Golub, Y. Xu, and G. Palmquist. "An ultracold neutron source at the NC State University PULSTAR reactor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 579, no. 1 (August 2007): 530–33. http://dx.doi.org/10.1016/j.nima.2007.04.116.

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Korobkina, E., G. Medlin, B. Wehring, A. I. Hawari, P. R. Huffman, A. R. Young, B. Beaumont, and G. Palmquist. "Ultracold neutron source at the PULSTAR reactor: Engineering design and cryogenic testing." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 767 (December 2014): 169–75. http://dx.doi.org/10.1016/j.nima.2014.08.016.

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Leach, Robert A., Patrick L. Parker, and Paul S. Veal. "PulStar differential compliance spinal instrument: a randomized interexaminer and intraexaminer reliability study." Journal of Manipulative and Physiological Therapeutics 26, no. 8 (October 2003): 493–501. http://dx.doi.org/10.1016/s0161-4754(03)00106-4.

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Datta, Arka, and Ayman I. Hawari. "Investigation of a model based reconstruction technique for neutron tomography at the PULSTAR reactor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 954 (February 2020): 161200. http://dx.doi.org/10.1016/j.nima.2018.09.035.

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Hathaway, A. G., M. Skalsey, W. E. Frieze, R. S. Vallery, D. W. Gidley, A. I. Hawari, and J. Xu. "Implementation of a prototype slow positron beam at the NC State University PULSTAR reactor." Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 579, no. 1 (August 2007): 538–41. http://dx.doi.org/10.1016/j.nima.2007.03.036.

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Dissertations / Theses on the topic "PULSTAR"

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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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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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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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Cameron, Andrew [Verfasser]. "Innovative Pulsar Searching Techniques : or Fantastic Pulsars and How to Find Them / Andrew Cameron." Bonn : Universitäts- und Landesbibliothek Bonn, 2018. http://d-nb.info/1162953063/34.

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Keane, Evan. "The transient radio sky." Thesis, University of Manchester, 2010. https://www.research.manchester.ac.uk/portal/en/theses/the-transient-radio-sky(37c08735-cd96-4598-a8b9-2d24ef9e871d).html.

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The high time-resolution radio sky represents unexplored astronomical territory where the discovery potential is high. In this thesis I have studied the transient radio sky, focusing on millisecond scales. As such, this work is concerned primarily with neutron stars, the most populous member of the radio transient parameter space. In particular, I have studied the well known radio pulsars and the recently identified group of neutron stars which show erratic radio emission, known as RRATs, which show radio bursts every few minutes to every few hours. When RRATs burst onto the scene in 2006, it was thought that they represented a previously unknown, distinct class of sporadically emitting sources. The difficulty in their identification implies a large underlying population, perhaps larger than the radio pulsars. The first question investigated in this thesis was whether the large projected population of RRATs posed a problem, i.e. could the observed supernova rate account for so many sources. In addition to pulsars and RRATs, the various other known neutron star manifestations were considered, leading to the conclusion that distinct populations would result in a 'birthrate problem'. Evolution between the classes could solve this problem - the RRATs are not a distinct population of neutron stars. Alternatively, perhaps the large projected population of RRATs is an overestimate. To obtain an improved estimate, the best approach is to find more sources. The Parkes Multi-beam Pulsar Survey, wherein the RRATs were initially identified, offered an opportunity to do just this. About half of the RRATs showing bursts during the survey were thought to have been missed, due to the deleterious effects of impulsive terrestrial interference signals. To remove these unwanted signals, so that we could identify the previously shrouded RRATs, we developed new interference mitigation software and processing techniques. Having done this, the survey was completely re-processed, resulting in the discovery of 19 new sources. Of these, 12 have been re-detected on multiple occasions, whereas the others have not been seen to re-emit since the initial discovery observations, and may be very low burst-rate RRATs, or, isolated burst events. These discoveries suggest that the initial population estimate was not over-estimated - RRATs, though not a distinct population, are indeed numerous. In addition to finding new sources, characterisation of their properties is vital. To this end, a campaign of regular radio observations of the newly discovered sources, was mounted, at the Parkes Observatory, in Australia. In addition, some of the initially identified RRATs were observed with the Lovell Telescope at Jodrell Bank. These have revealed glitches in J1819-1458, with anomalous post-glitch recovery of the spin-down rate. If such glitches were common, it would imply that the source was once a magnetar, neutron stars with the strongest known magnetic fields of up to 10¹⁵ gauss. The observations have also been used to perform 'timing' observations of RRATs, i.e. determination of their spin-down characteristics. At the beginning of this thesis, 3 of the original sources had 'timing solutions' determined. This has since risen to 7, and furthermore, 7 of the newly discovered sources now also have timing solutions. With this knowledge, we can see where RRATs lie in period-period derivative space. The Parkes RRATs seem to be roughly classifiable into three groupings, with high observed nulling fractions - normal pulsars, high magnetic field pulsars and old, 'dying' pulsars. It seems that RRATs and pulsars are one and the same. When a pulsar is more easily detected in searches for single bright pulses, as opposed to in periodicity searches, we label it a RRAT. Such searches impart a selection effect on the parameter space of possible sources, in both nulling fraction and rotation period. In this sense, an observational setup could be designed to make any pulsar appear as a RRAT. For realistic survey parameters however, this is not the case, and the groups mentioned above seem to be the most likely to appear as RRATs. In fact, we can utilise RRAT searches to identify neutron stars, difficult to find by other means, in particular high-magnetic field pulsars, and pulsars approaching the pulsar "death valley". Some of the RRATs are well explained as being distant/weak pulsars with a high modulation index, others seem to be nulling pulsars. This highlights the incomplete knowledge of nulling behaviour in the pulsar population. It seems that there may be a continuum of nulling durations, under a number of guises, from 'nulling pulsars' to 'RRATs' to 'intermittent pulsars'. In fact this nulling may fit into the emerging picture, whereby pulsar magnetospheres switch between stable configurations.
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Venter, Christo. "Millisecond pulsars and pulsar wind nebulae as sources of gamma rays and cosmic rays / C. Venter." Thesis, North-West University, 2008. http://hdl.handle.net/10394/2067.

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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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Bondonneau, Louis. "Première caractérisation de la population de pulsars radio à basses fréquences avec NenuFAR." Thesis, Orléans, 2019. http://www.theses.fr/2019ORLE3032.

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Un pulsar est une étoile à neutrons en rotation rapide (typiquement un tour par seconde) dont le faisceau d’émission radio provenant des pôles magnétiques de l'étoile balaie l’univers. Quand le faisceau intercepte la Terre, le pulsar est détectable comme une série de pulsations régulières dans dans un vaste domaine de longueurs d'onde, de la radio jusqu'aux rayons gamma. Au cours de cette thèse j’ai utilisé, adapté et développé des méthodes d'analyses ainsi qu'un pipeline de traitement de signal en temps réel afin d’étudier les signaux radio des pulsars dans la gamme des basses fréquences utilisée par les radiotélescopes LOFAR(LOw Frequency Array) et NenuFAR (New Extension in Nançay Upgrading loFAR).NenuFAR est le nouvel instrument de la station de Radioastronomie de Nançay, construit pour observer le ciel entre 10 et 85 MHz de fréquence. C'est un réseau compact de nouvelle génération, constitué à terme de 1938 antennes phasées analogiquement et numériquement. Depuis le début de ma thèse, j'ai participé activement au développement, puis à la recette de ce nouvel instrument, jusqu'à son ouverture à la communauté scientifique le 1er juillet 2019 dans le cadre d’un appel à "Early Science".Le premier chapitre de ma thèse est consacré à la description du phénomène « pulsar », de l'émission du rayonnement dans la magnétosphère de l'étoile à neutrons jusqu'à l'observation du signal par le radiotélescope. Le second chapitre décrit l’instrumentation des radiotélescopes utilisés pendant la thèse, et en particulier, la conception du dédisperseur « pulsar » cohérent en temps réel de NenuFAR (LUPPI) et du « pipeline » de traitement des observations. Le troisième chapitre est réservé à l’étude d’une centaine de pulsars observés à basse fréquence avec LOFAR. Les données sont issues de deux relevés, l’un effectué avec le coeur de LOFAR (situé aux Pays-Bas) et l’autre avec la station LOFAR de Nançay. Finalement, le dernier chapitre est dédié à la mise en service de NenuFAR et aux premiers résultats scientifiques obtenus pour les observations des pulsars. Ce chapitre décrit en particulier les tests pour les différents modes d'observation (dédispersion cohérente, multi-beam, single pulse, enregistrement en forme d'onde) et le résultat du premier grand relevé du ciel Nord par NenuFAR, qui a permis à partir de l’observation de 500 pulsars la détection de 130 sources, dont plus de 50 pour la première fois à ces fréquences. J'y présente également le programme scientifique du projet clé pulsars de NenuFAR, que j'ai fortement contribué à mettre en place
A pulsar is a rapidly rotating neutron star (typically one revolution per second). As it rotates, the beamed radio emission from the star's magnetic poles scans the universe. When the beam intercepts the Earth, the pulsar is detectable as a series of regular pulses over a wide wavelength range, from radio to gamma rays. During this thesis I used, adapted and developed analysis methods and a real-time signal processing pipeline to study pulsar radio signals in the low frequency range used by the radio telescopes LOFAR (LOw Frequency Array) and NenuFAR (New Extension in Nançay Upgrading loFAR).NenuFAR is the new instrument of the Nançay Radio Astronomy Station, built to observe the sky at frequency between 10 and 85 MHz. It is a compact array of the last generation of radio telescopes. Ultimately it will be composed of 1938 antennas with analog and digital phasing. Since the beginning of my thesis, I have been actively involved in the development of this new instrument, until it was opened to the scientific community on July 1, 2019 as part of a call for "Early Science".The first chapter of my thesis is devoted to the description of the "pulsar" phenomenon, from the emission of radiation in the magnetosphere of the neutron star to the observation of the signal by a radio telescope. The second chapter describes the instrumentation of the radio telescopes used during the thesis, and in particular the design of the NenuFAR coherent real-time "pulsar" dedispersion system (LUPPI) and the pipeline for the processing of the observations. The third chapter presents the study of about 100 pulsars observed at low frequency with LOFAR. The data are based on two surveys, one with the LOFAR core (located in the Netherlands) and the other with the LOFAR station in Nançay. Finally, the last chapter is dedicated to the commissioning of NenuFAR and the first scientific results obtained from pulsars observations. This chapter describes in particular the tests for the different observation modes (coherent dedispersion, multi-beam, single pulse, waveform recording) and the result of the first major survey of the North sky by NenuFAR. Based on the observation of 500 pulsars, this survey allowed the detection of 130 sources, including more than 50 which had never been detected at these frequencies before. I also present the scientific program of the NenuFAR pulsar Key Project, to which I have strongly contributed
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Edwards, Russell T., and Russell Edwards@csiro au. "Pulsar searching." Swinburne University of Technology, 2001. http://adt.lib.swin.edu.au./public/adt-VSWT20050323.141044.

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This thesis reports the results of two pulsar survey projects conducted at the Parkes 64-m radio telescope in New South Wales, Australia. The first, the Swinburne Intermediate Latitude Pulsar Survey, covered a large region of the southern Galaxy flanking that of the ongoing Galactic plane survey. We used the 13-feed 20 cm 'multibeam' receiver package to achieve this broad sky coverage in a short observing campaign with 14 days� total integration time. The survey proved remarkably successful, detecting 170 pulsars, 69 of which were new discoveries. Eight of the new discoveries possess small periods and period derivatives indicative of 'recycling', an hypothesis supported by the fact that six of them are in circular orbits with probable white dwarf companions. Pulse timing measurements have revealed that two of the white dwarfs are massive CO or ONeMg dwarfs. The mass of one of them (the companion to PSR J1157�5112) exceeds 1.14 M, providing the most convincing evidence to date for the production of 'ultra-massive' ONeMg white dwarfs as the end result of stellar evolution on the asymptotic giant branch (albeit with mass transfer indicated). PSR J1757�5322 also possesses a heavy white dwarf companion, in a close 11-h orbit. The proximity of the massive companion leads to significant relativistic orbital evolution and the effects of this will be measurable by pulsar timing in the coming decades. Under general relativity, the gravitational wave power radiated from the system is sufficient to cause coalescence in an event which will have dramatic and unknown consequences. Such events are possible gamma-ray burst sources, and the remnants could include isolated millisecond pulsars, close eclipsing binaries or pulsar planetary systems. The remaining four pulsar binaries show some discrepancies with the bulk of previously known low mass binary pulsars (LMBPs). PSR J1618-39 is in a 23-d orbit, filling what previously appeared to be a gap in the orbital period distribution. PSR J1745-0952 has a relatively long pulse period (19 ms) and along with PSR J1618-39 (12 ms) may have experienced a different evolutionary history to the majority of previously known LMBPs. A ninth pulsar discovered in the survey may also be recycled. The mean pulse profile of PSR J1411�7404 is exceedingly narrow and lies in stark contrast to that of other pulsars of similar pulse period. In the past the only other pulsars known with anomalously narrow profiles were believed (for other reasons) to have been recycled, and this fact in combination with the low period derivative measured in timing analysis of PSR J1411�7404 leads me to suggest that it, too, may have been recycled. If this is the case, it is possible that the recycling took place in a system similar in configuration to the progenitors of the double neutron star systems, but that sudden mass loss or an unfavourably oriented kick in the birth event of the second neutron star disrupted the system, leaving an isolated, mildly recycled pulsar. The second pulsar survey program conducted for this work was a targeted search of southern globular clusters. We used a baseband recording system to provide unprecedented time resolution (typically 25 �s). The large number of channels and short sampling interval achievable in software filterbanks, in combination with the ability to coherently remove most of the interstellar dispersion from clusters with previously known pulsars, made us the first to achieve a relatively flat sensitivity response to pulsars of ~10−3.5�10 s. This characteristic is vital if we are to constrain the true period distribution of millisecond pulsars, an important task in the evaluation of alternative equations of state for nuclear matter. We detected six millisecond pulsars and produced pulse profiles of higher resolution than were previously available. The basic sensitivity of the search was not high enough to detect any new pulsars, however the work demonstrates that the approach is feasible with the use of currently available high-performance computing resources (such as the Swinburne workstation cluster), and is capable of delivering excellent sensitivity characteristics. It is expected that future searches of this kind, of which this is the first, will achieve the goal of sampling the true pulse period distribution within a few years.
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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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Books on the topic "PULSTAR"

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1923-, Graham-Smith Francis Sir, ed. Pulsar astronomy. 4th ed. Cambridge: Cambridge University Press, 2012.

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1923-, Graham-Smith Francis Sir, ed. Pulsar astronomy. 3rd ed. Cambridge: Cambridge University Press, 2006.

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Lyne, A. G. Pulsar astronomy. 2nd ed. Cambridge: Cambridge University Press, 1998.

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Lyne, A. G. Pulsar astronomy. Cambridge [England]: Cambridge University Press, 1989.

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Kadomt︠s︡ev, B. B. On the pulsar. Singapore: World Scientific, 2010.

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Kadomt︠s︡ev, B. B. On the pulsar. New Jersey: World Scientific, 2009.

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On the pulsar. New Jersey: World Scientific, 2009.

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Kadomt︠s︡ev, B. B. On the pulsar. New Jersey: World Scientific, 2009.

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Le dernier pulsar. Montréal: La Courte échelle, 2011.

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On the pulsar. New Jersey: World Scientific, 2009.

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Book chapters on the topic "PULSTAR"

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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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Vink, Jacco. "Neutron Stars, Pulsars, and Pulsar Wind Nebulae." In Astronomy and Astrophysics Library, 117–69. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-55231-2_6.

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Cheng, Kwong Sang. "High Energy Emission from Pulsars and Pulsar Wind Nebulae." In Neutron Stars and Pulsars, 481–520. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76965-1_18.

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Wilhelmi, Emma de Oña. "Cherenkov Telescopes Results on Pulsar Wind Nebulae and Pulsars." In High-Energy Emission from Pulsars and their Systems, 435–52. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-17251-9_37.

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Prantzos, Nikos. "Pulsar." In Encyclopedia of Astrobiology, 1386–87. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1308.

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Prantzos, Nikos. "Pulsar." In Encyclopedia of Astrobiology, 1. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_1308-3.

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Prantzos, Nikos. "Pulsar." In Encyclopedia of Astrobiology, 2088–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 2015. http://dx.doi.org/10.1007/978-3-662-44185-5_1308.

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Wolszczan, Alexander. "Pulsar Planets." In Encyclopedia of Astrobiology, 1387–89. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-11274-4_1309.

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Wolszczan, Alexander. "Pulsar Planets." In Encyclopedia of Astrobiology, 1–5. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-27833-4_1309-2.

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Bailes, Matthew. "Pulsar Velocities." In Compact Stars in Binaries, 213–23. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-0167-4_17.

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Conference papers on the topic "PULSTAR"

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Liu, M., and A. I. Hawari. "The upgraded intense positron beam facility at the PULSTAR reactor." In INTERNATIONAL CONFERENCE ON SCIENCE AND APPLIED SCIENCE (ICSAS) 2019. AIP Publishing, 2019. http://dx.doi.org/10.1063/1.5135840.

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Hawari, A., and S. Lassell. "Internet Reactor Laboratory (IRL): Nuclear Engineering Education Utilizing the PULSTAR Reactor." In Tranactions - 2019 Winter Meeting. AMNS, 2019. http://dx.doi.org/10.13182/t31117.

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Xiao, Ziyu, and Ayman I. Hawari. "Design considerations of a coded source neutron imaging system at the PULSTAR reactor." In 2011 IEEE Nuclear Science Symposium and Medical Imaging Conference (2011 NSS/MIC). IEEE, 2011. http://dx.doi.org/10.1109/nssmic.2011.6154537.

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Hawari, Ayman I., David W. Gidley, Jun Xu, Jeremy Moxom, Alfred G. Hathaway, Benjamin Brown, Richard Vallery, Floyd D. McDaniel, and Barney L. Doyle. "The Intense Slow Positron Beam Facility at the NC State University PULSTAR Reactor." In APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: Twentieth International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3120175.

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Moxom, Jeremy, Alfred G. Hathaway, and Ayman I. Hawari. "Out of core testing of the North Carolina State University PULSTAR reactor positron beam." In 2007 IEEE Nuclear Science Symposium Conference Record. IEEE, 2007. http://dx.doi.org/10.1109/nssmic.2007.4436615.

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Ziyu Xiao, K. K. Mishra, A. I. Hawari, H. Z. Bilheux, P. R. Bingham, and K. W. Tobin. "Investigation of coded source neutron imaging at the north carolina state university PULSTAR reactor." In 2009 IEEE Nuclear Science Symposium and Medical Imaging Conference (NSS/MIC 2009). IEEE, 2009. http://dx.doi.org/10.1109/nssmic.2009.5402357.

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Liu, Ming, Jeremy Moxom, Ayman I. Hawari, and David W. Gidley. "The intense slow positron beam facility at the PULSTAR reactor and applications in nano-materials study." In APPLICATION OF ACCELERATORS IN RESEARCH AND INDUSTRY: Twenty-Second International Conference. AIP, 2013. http://dx.doi.org/10.1063/1.4802370.

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Lobato, Ronaldo V., J. G. Coelho, and M. Malheiro. "Radio pulsar death lines to SGRs/AXPs and white dwarfs pulsars." In THE SECOND ICRANET CÉSAR LATTES MEETING: Supernovae, Neutron Stars and Black Holes. AIP Publishing LLC, 2015. http://dx.doi.org/10.1063/1.4937186.

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Dolch, Timothy. "Pulsars at Low Radio Frequencies, Cyclic Spectroscopy, and Pulsar Timing Arrays." In 2019 United States National Committee of URSI National Radio Science Meeting (USNC-URSI NRSM). IEEE, 2019. http://dx.doi.org/10.23919/usnc-ursi-nrsm.2019.8712895.

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Kijak, J., W. Lewandowski, M. Serylak, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Turn-over in pulsar spectra: From young pulsars to millisecond ones." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900132.

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Reports on the topic "PULSTAR"

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Perez, P. B., and S. J. Bilyj. NCSU PULSTAR Reactor instrumentation upgrade. Office of Scientific and Technical Information (OSTI), August 1993. http://dx.doi.org/10.2172/10188894.

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Mayo, C. W., K. Verghese, and Y. G. Huo. Mixed enrichment core design for the NC State University PULSTAR Reactor. Office of Scientific and Technical Information (OSTI), December 1997. http://dx.doi.org/10.2172/319770.

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Bilyj, S. J., and P. B. Perez. NCSU PULSTAR reactor instrumentation upgrade. Final technical report, September 6, 1990--March 19, 1993. Office of Scientific and Technical Information (OSTI), November 1993. http://dx.doi.org/10.2172/10120629.

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Perez, P. B. Upgrade of the NCSU PULSTAR instrumentation power channels. Final technical report, September 1, 1992--August 31, 1994. Office of Scientific and Technical Information (OSTI), November 1998. http://dx.doi.org/10.2172/296822.

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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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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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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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Bulos, Fatin. Kicker Magnet and Pulser. Office of Scientific and Technical Information (OSTI), March 2014. http://dx.doi.org/10.2172/1122490.

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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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Spitkovsky, Anatoly. Time-dependent Force-free Pulsar Magnetospheres: Axisymmetric and Oblique Rotators. Office of Scientific and Technical Information (OSTI), April 2006. http://dx.doi.org/10.2172/881123.

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