Relevant bibliographies by topics / Pulsar timing

Academic literature on the topic 'Pulsar timing'

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Published: 4 June 2021
Last updated: 13 February 2022

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Journal articles on the topic "Pulsar timing"

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MANCHESTER, R. N. "PULSAR SEARCHING AND TIMING." International Journal of Modern Physics D 22, no. 01 (January 2013): 1341007. http://dx.doi.org/10.1142/s0218271813410071.

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More than 2000 pulsars are now known. These pulsars may be divided into a number of different classes according to their period, period derivative, binary properties, emission characteristics and so on. Some important classes have relatively few members, e.g. double-neutron-star binary systems, and so continued searches for currently unknown pulsars are important. Such searches are being undertaken at various observatories around the world. Somewhat unexpectedly, the Fermi Gamma-ray Observatory, has proved to be an efficient pulsar detector, especially for millisecond pulsars (MSPs). The great stability of pulsar periods, especially for MSPs, leads to a number of important applications of pulsar timing. The detection and study of relativistic orbit perturbations in double-neutron-star systems has proved to be a powerful tool with measurements of the original binary pulsar, PSR B1913+16, and more recently the double pulsar, PSR J0737-3039A/B, showing that Einstein's general theory of relativity accurately describes these gravitational interactions. Direct detection of gravitational waves using pulsar timing is close to being achieved with the development of pulsar timing arrays (PTAs) in Europe, North America and Australia. Combining data from these PTAs to form the International Pulsar Timing Array (IPTA) will lead to improved significance of such a detection. Ultimately, detailed study of gravitational-wave sources will be possible using future large radio telescopes such as FAST and the SKA.
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Rodin, Alexander E. "Pulsar timing array." Proceedings of the International Astronomical Union 5, H15 (November 2009): 229–30. http://dx.doi.org/10.1017/s1743921310008951.

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AbstractSimultaneous timing of several pulsars distributed over the sky, so called Pulsar Timing Array (PTA), is used for a variety of metrological and astronomical applications. Three examples of PTA application are presented: link between celestial reference frames, ensemble pulsar time scale and detection of gravitational waves.
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McLaughlin, Maura. "Pulsar Timing Arrays." Proceedings of the International Astronomical Union 11, A29B (August 2015): 321–28. http://dx.doi.org/10.1017/s1743921316005457.

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AbstractI describe the concept of a pulsar timing array and give broad overview of the construction of a pulsar timing array, methods for high-precision timing and noise characterization, and algorithms for gravitational wave detection and source characterization. I then provide an overview of worldwide pulsar timing programs and the scale and sensitivity of the pulsar timing array efforts, with particular attention to the International Pulsar Timing Array (IPTA). I discuss the most recent results from pulsar timing arrays, emphasizing the gravitational wave detection efforts in particular. Finally, I describe the anticipated future growth in participants, telescopes, pulsars, and sensitivity of the IPTA, highlighting the transformational advances that it will enable over the next decade.
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Reardon, D. J., R. M. Shannon, A. D. Cameron, B. Goncharov, G. B. Hobbs, H. Middleton, M. Shamohammadi, et al. "The Parkes pulsar timing array second data release: timing analysis." Monthly Notices of the Royal Astronomical Society 507, no. 2 (August 11, 2021): 2137–53. http://dx.doi.org/10.1093/mnras/stab1990.

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ABSTRACT The main goal of pulsar timing array experiments is to detect correlated signals such as nanohertz-frequency gravitational waves. Pulsar timing data collected in dense monitoring campaigns can also be used to study the stars themselves, their binary companions, and the intervening ionized interstellar medium. Timing observations are extraordinarily sensitive to changes in path-length between the pulsar and the Earth, enabling precise measurements of the pulsar positions, distances and velocities, and the shapes of their orbits. Here we present a timing analysis of 25 pulsars observed as part of the Parkes Pulsar Timing Array (PPTA) project over time spans of up to 24 yr. The data are from the second data release of the PPTA, which we have extended by including legacy data. We make the first detection of Shapiro delay in four Southern pulsars (PSRs J1017−7156, J1125−6014, J1545−4550, and J1732−5049), and of parallax in six pulsars. The prominent Shapiro delay of PSR J1125−6014 implies a neutron star mass of Mp = 1.5 ± 0.2 M⊙ (68 per cent credibility interval). Measurements of both Shapiro delay and relativistic periastron advance in PSR J1600−3053 yield a large but uncertain pulsar mass of $M_p = 2.06^{+0.44}_{-0.41}$ M⊙ (68 per cent credibility interval). We measure the distance to PSR J1909−3744 to a precision of 10 lyr, indicating that for gravitational wave periods over a decade, the pulsar provides a coherent baseline for pulsar timing array experiments.
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Yang, Tinggao, and Guangren Ni. "Ensemble Pulsar Time Study by Pulsar Timing Observations." Symposium - International Astronomical Union 218 (2004): 439–40. http://dx.doi.org/10.1017/s0074180900181604.

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Long term timing of multiple millisecond pulsars can contribute to the study of an ensemble pulsar time scale PTens. A wavelet decomposition algorithm (WDA) was applied to define a PTens using the available millisecond pulsar timing datA. The PTens obtained from WDA is more stable than those resulting from other algorithms. The Chinese 50 m radio telescope is specially designed for PTens study and detection of gravitational wave background via millisecond pulsars timing observations. A scheme for multiple millisecond pulsar timing and ensemble pulsar time study is discussed in some detail.
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Lower, M. E., M. Bailes, R. M. Shannon, S. Johnston, C. Flynn, S. Osłowski, V. Gupta, et al. "The UTMOST pulsar timing programme – II. Timing noise across the pulsar population." Monthly Notices of the Royal Astronomical Society 494, no. 1 (March 4, 2020): 228–45. http://dx.doi.org/10.1093/mnras/staa615.

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ABSTRACT While pulsars possess exceptional rotational stability, large-scale timing studies have revealed at least two distinct types of irregularities in their rotation: red timing noise and glitches. Using modern Bayesian techniques, we investigated the timing noise properties of 300 bright southern-sky radio pulsars that have been observed over 1.0–4.8 yr by the upgraded Molonglo Observatory Synthesis Telescope (MOST). We reanalysed the spin and spin-down changes associated with nine previously reported pulsar glitches, report the discovery of three new glitches and four unusual glitch-like events in the rotational evolution of PSR J1825−0935. We develop a refined Bayesian framework for determining how red noise strength scales with pulsar spin frequency (ν) and spin-down frequency ($\dot{\nu }$), which we apply to a sample of 280 non-recycled pulsars. With this new method and a simple power-law scaling relation, we show that red noise strength scales across the non-recycled pulsar population as $\nu ^{a} |\dot{\nu }|^{b}$, where $a = -0.84^{+0.47}_{-0.49}$ and $b = 0.97^{+0.16}_{-0.19}$. This method can be easily adapted to utilize more complex, astrophysically motivated red noise models. Lastly, we highlight our timing of the double neutron star PSR J0737−3039, and the rediscovery of a bright radio pulsar originally found during the first Molonglo pulsar surveys with an incorrectly catalogued position.
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Perera, B. B. P., M. E. DeCesar, P. B. Demorest, M. Kerr, L. Lentati, D. J. Nice, S. Osłowski, et al. "The International Pulsar Timing Array: second data release." Monthly Notices of the Royal Astronomical Society 490, no. 4 (October 12, 2019): 4666–87. http://dx.doi.org/10.1093/mnras/stz2857.

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ABSTRACT In this paper, we describe the International Pulsar Timing Array second data release, which includes recent pulsar timing data obtained by three regional consortia: the European Pulsar Timing Array, the North American Nanohertz Observatory for Gravitational Waves, and the Parkes Pulsar Timing Array. We analyse and where possible combine high-precision timing data for 65 millisecond pulsars which are regularly observed by these groups. A basic noise analysis, including the processes which are both correlated and uncorrelated in time, provides noise models and timing ephemerides for the pulsars. We find that the timing precisions of pulsars are generally improved compared to the previous data release, mainly due to the addition of new data in the combination. The main purpose of this work is to create the most up-to-date IPTA data release. These data are publicly available for searches for low-frequency gravitational waves and other pulsar science.
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Liu, Kuo. "Update on the European Pulsar Timing Array." Proceedings of the International Astronomical Union 8, S291 (August 2012): 180. http://dx.doi.org/10.1017/s1743921312023575.

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AbstractThe European Pulsar Timing Array (EPTA) is one the of three global Pulsar Timing Array communities, aiming to use the clock nature of pulsars to detect gravitational wave. In this talk, I will provide an introduction to the current status of EPTA pulsar observations and present an overview of the recent results. I will also give an update on the progress of the Large European Array for Pulsar (LEAP) project, which attempts to coherently combine the data from the five biggest single site radio telescopes in Europe and make an equivalently 200-metre diameter dish. The LEAP project is an ideal effort in performing high precision pulsar timing and studying characteristics of single pulses from millisecond pulsars.
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Hobbs, G. "Pulsar timing array projects." Proceedings of the International Astronomical Union 5, S261 (April 2009): 228–33. http://dx.doi.org/10.1017/s1743921309990445.

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AbstractPulsars are amongst the most stable rotators known in the Universe. Over many years some millisecond pulsars rival the stability of atomic clocks. Comparing observations of many such stable pulsars may allow the first direct detection of gravitational waves, improve the Solar System planetary ephemeris and provide a means to study irregularities in terrestrial time scales. Here we review the goals and status of current and future pulsar timing array projects.
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Manchester, R. N., A. G. Lyne, F. Camilo, V. M. Kaspi, I. H. Stairs, F. Crawford, D. J. Morris, J. F. Bell, and N. D’Amico. "Timing the Parkes Multibeam Pulsars." International Astronomical Union Colloquium 177 (2000): 49–54. http://dx.doi.org/10.1017/s0252921100058991.

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AbstractMeasurement of accurate positions, pulse periods and period derivatives is an essential follow-up to any pulsar survey. The procedures being used to obtain timing parameters for the pulsars discovered in the Parkes multibeam pulsar survey are described. Completed solutions have been obtained so far for about 80 pulsars. They show that the survey is preferentially finding pulsars with higher than average surface dipole magnetic fields. Eight pulsars have been shown to be members of binary systems and some of the more interesting results relating to these are presented.
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Dissertations / Theses on the topic "Pulsar timing"

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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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Mingarelli, Chiara Maria Francesca. "Gravitational wave astrophysics with pulsar timing arrays." Thesis, University of Birmingham, 2014. http://etheses.bham.ac.uk//id/eprint/5117/.

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This thesis focuses on gravitational wave (GW) astrophysics with Pulsar Timing Arrays (PTAs). Firstly it is shown that anisotropy in the GW background may be present, and that its characterization at different angular scales carries important information. The standard analysis for isotropic backgrounds is then generalized by decomposing the angular distribution of the GW energy density into multipole moments. Generalized overlap reduction functions (ORFs) are computed for a generic level of anisotropy and PTA configuration. A rigorous analysis is then done of the assumptions made when calculating ORFs. It is shown that correlated phase changes introduce previously unmodeled effects for pulsars pairs separated by less than a radiation wavelength. The research then turns to the study of continuous GW sources from supermassive black hole binaries (SMBHBs). Here it shown that the detection of GWs from SMBHB systems can yield direct information about the masses and spins of the black holes, provided that the GW-induced timing fluctuations both at the pulsar and at Earth are detected. This in turn provides a map of the nonlinear dynamics of the gravitational field and a new avenue to tackle open problems in astrophysics connected to the formation and evolution of SMBHs.
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Hemberger, Daniel. "Improving Pulsar Timing through Interstellar Scatter Correction." Oberlin College Honors Theses / OhioLINK, 2007. http://rave.ohiolink.edu/etdc/view?acc_num=oberlin1207521228.

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Van, Straten Willem Herman Bernadus, and straten@astron nl. "High-Precision timing and polarimeter of PSR JO437-4715." Swinburne University of Technology. School of Biophysical Sciences and electrical Engineering, 2003. http://adt.lib.swin.edu.au./public/adt-VSWT20040311.123754.

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This thesis reports on the recent results of a continuing, high-precision pulsar timing project, currently focused on the nearby, binary millisecond pulsar, PSR J0437_4715. Pulse arrival time analysis has yielded a remarkable series of constraints on the physical parameters of this system and evidence for the distortion of space-time as predicted by the General Theory of Relativity. Owing to the proximity of the PSR J0437_4715 system, relative changes in the positions of the Earth and pulsar result in both annual and secular evolution of the line of sight to the pulsar. Although the changes are miniscule, the effects on the projected orbital parameters are detectable in our data at a high level of significance, necessitating the implementation of an improved timing model. In addition to producing estimates of astrometric parameters with unparalleled precision, the study has also yielded the first three-dimensional orbital geometry of a binary pulsar. This achievement includes the first classical determination of the orbital inclination, thereby providing the unique opportunity to verify the shape of the Shapiro delay and independently confirm a general relativistic prediction. With a current post-fit arrival time residual RMS of 130 ns over four years, the unrivaled quality of the timing data presented herein may eventually contribute to the most stringent limit on the energy density of the proposed stochastic gravitational wave background. Continuing the quest for even greater timing precision, a detailed study of the polarimetry of PSR J0437_4715 was undertaken. This effort culminated in the development of a new, phase-coherent technique for calibrating the instrumental response of the observing system. Observations were conducted at the Parkes 64-m radio telescope in New South Wales, Australia, using baseband recorder technologies developed at York University, Toronto, and at the California Institute of Technology. Data were processed off-line at Swinburne University using a beowulf-style cluster of high-performance workstations and custom software developed by the candidate as part of this thesis.
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Sakai, Satoru. "The effect of Shapiro delay on pulsar timing." Thesis, University of Glasgow, 2011. http://theses.gla.ac.uk/3020/.

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Light passing near a massive object (star) will take longer to arrive at the Earth than it would if the object was not present. This additional time is called the Shapiro delay. In globular clusters, where there are millions of stars, the cumulative effect of the Shapiro delay from these stars will affect pulsar timings by introducing an additional noise term. This effect has been previously assumed to be small, yet no definite investigation has been done to determine its magnitude. In this thesis a model of the globular cluster 47 Tucanae was created in order to determine the effect of the change in Shapiro delay (called the Shapiro noise) for an observed duration of 3600 days -- the current longest observation period for pulsar timing. This noise was then added to the pulsar time of arrival (TOA) as the only noise source in pulsar timing. A polynomial fit was then used to subtract the first two orders from the pulse arrival time (the f and \dot{f} terms) to determine the timing residuals. This model was then realised 100 times to obtain the average root mean square (RMS) timing residual for every pulsar. The model showed that the Shapiro noise has a significant, and observable effect on pulsar timing, especially for pulsars situated close to the core of the globular cluster. From the model the average RMS timing residuals were of the order of 10^{-5} to 10^{-7} seconds and the variance of the RMS timing residuals were significantly larger in magnitude, ranging from 10^{-4} to 10^{-7} seconds for every pulsar. The importance of this result motivated further investigation of the stellar distribution of the globular cluster. In addition an investigation on how the effect of gravitational acceleration (produced by stars situated close to the pulsar) affects pulsar timing residual was also done. While the acceleration has an effect, the effect is smaller than that of the Shapiro noise. From the timing residuals produced by the Shapiro noise, it was then discussed whether any star close to the LOS would have an affect on the pulsar timing residuals. From additional simulations it was determined that stars anywhere along the LOS will have an affect on pulsar timing, however the stellar density of such a region would have to be greater than \rho_{min} > 10^{5} M_{\sun} pc^{-3}. The implications of this result for other pulsars in (other) globular clusters is discussed.
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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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Grandy, Victoria Rebecca. "Wideband timing of the double pulsar (PSR J0737-3039A)." Thesis, University of British Columbia, 2016. http://hdl.handle.net/2429/59959.

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Pulsars are neutron stars (NS) that produce beamed radio-frequency emission. Due to their rapid, steady rotation rate, this signal is detected as a series of pulses whose integrated profile is unusually stable over time. Pulsars in double neutron star (DNS) binary systems are a rare, but extremely useful, astronomical tool and have been used in tests of gravity theories in the strong-gravitational field limit. Rarer still are DNS systems in which both objects have been detected as pulsars; only one such system has been found thus far -- PSR J0737-3039A/B. Discovered over a decade ago, this system consists of one recycled pulsar, PSR J0737-3039A, and its companion, PSR J0737-3039B, which has since become undetectable. In any pulsar-related research, precise timing is necessary to produce meaningful results. The pulse time of arrivals (TOAs) are greatly affected by the medium through which the electromagnetic (EM) signal travels in both frequency-dependent and -independent ways. Even after accounting for such effects, many pulse profiles still exhibit frequency-dependent shape changes, which can greatly affect the precision of the timing results. Traditionally, corrections are applied to the TOAs after calculation in an ad hoc manner. In contrast to this, we explored the wideband timing algorithm developed by Timothy T. Pennucci and collaborators which accounts for frequency-dependent profile changes through a two-dimensional Gaussian pulse portrait model implemented in the TOA calculations. It was found that the portrait model is well-representative of the pulse profile shape over a wide frequency range. This method is also able to produce a robust set of wideband TOAs. The subsequent timing model, determined with TEMPO timing software, was found to be comparable to those produced from subbanded TOAs derived though more traditional methods. Some inconsistencies between the timing model astrometric and spin parameters of the wideband and subbanded data of this well-studied pulsar imply potential difficulties in achieving precise timing results not only for this pulsar, but for others, such as those used in pulsar timing arrays aiming to detect gravitational waves.
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Middleton, Hannah Rose. "Astrophysical inference from pulsar timing array searches for gravitational waves." Thesis, University of Birmingham, 2018. http://etheses.bham.ac.uk//id/eprint/8044/.

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Gravitational waves (GWs) have been detected for the first time in 2015 by the LIGO-Virgo Scientific Collaboration. The source of the GWs was a binary black hole (BBH). The observation caught the final fraction of a second as the two black holes spiralled together and merged. This observation (and the others to follow) marked the beginnings of GW astronomy, ‘a new window on the dark universe’, providing a means to observe astronomical phenomena which may be completely inaccessible via other avenues as well as a new testing ground for Einstein’s theory of general relativity (GR). However, this is just the beginning – like electromagnetic astrophysics, there is a full spectrum of GW frequencies to explore. At very low frequencies, pulsar timing arrays (PTAs) are being used to search for the GW background from the merging population of massive black hole binaries (MBHBs). No detection has yet been made, but upper limits have been placed. Here we present results on what inference on the MBHB population can be learnt from present and possible future PTA results, and also compare current upper limits with astrophysical predictions, finding them to be fully consistent so far. We also present a generic method for testing the consistency of a theory against experimental evidence in the situation where there is no strong viable alternative (for example GR). We apply this to BBH observations, finding them to be fully consistent with GR and also to Newton’s constant of gravitation, where there is considerable inconsistency between measurements.
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NG, Wing Yan [Verfasser]. "Pulsar searching and timing with the Parkes telescope / Wing Yan NG." Bonn : Universitäts- und Landesbibliothek Bonn, 2014. http://d-nb.info/1077289022/34.

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Caballero, Pouroutidou Ricardo Nicolaos [Verfasser]. "Probing Gravity with High-Precision Pulsar Timing / Ricardo Nicolaos Caballero Pouroutidou." Bonn : Universitäts- und Landesbibliothek Bonn, 2016. http://d-nb.info/1124540318/34.

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Books on the topic "Pulsar timing"

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Mingarelli, Chiara M. F. Gravitational Wave Astrophysics with Pulsar Timing Arrays. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-18401-2.

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van Haasteren, Rutger. Gravitational Wave Detection and Data Analysis for Pulsar Timing Arrays. Berlin, Heidelberg: Springer Berlin Heidelberg, 2014. http://dx.doi.org/10.1007/978-3-642-39599-4.

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3

Audley, Michael Damian. A broad-band spectral and timing study of the X-ray binary system Centaurus X-3. Greenbelt, Md: Laboratory for High Energy Astrophysics, National Aeronautics and Space Administration, Goddard Space Flight Center, 1998.

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Audley, Michael Damian. A broad-band spectral and timing study of the X-ray binary system Centaurus X-3. Greenbelt, Md: Laboratory for High Energy Astrophysics, National Aeronautics and Space Administration, Goddard Space Flight Center, 1998.

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Audley, Michael Damian. A broad-band spectral and timing study of the X-ray binary system Centaurus X-3. Greenbelt, Md: Laboratory for High Energy Astrophysics, National Aeronautics and Space Administration, Goddard Space Flight Center, 1998.

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Audley, Michael Damian. A broad-band spectral and timing study of the X-ray binary system Centaurus X-3. Greenbelt, Md: Laboratory for High Energy Astrophysics, National Aeronautics and Space Administration, Goddard Space Flight Center, 1998.

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van, Paradijs J., Maitzen H. M. 1943-, and European Astrophysics Doctoral Network, eds. Galactic high-energy astrophysics ; High-accuracy timing and positional astronomy: Lectures held at the Astrophysics School IV, organized by the European Astrophysics Doctoral Network (EADN) in Graz, Austria, 19-31 August 1991. Berlin: Springer-Verlag, 1993.

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Maggiore, Michele. Stochastic backgrounds and pulsar timing arrays. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198570899.003.0014.

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Chiara M. F. M. F. Mingarelli. Gravitational Wave Astrophysics with Pulsar Timing Arrays. Springer, 2015.

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Trustees, Columbia University, Columbia Astrophysics Laboratory (Columbia University), Compton Observatory, and United States. National Aeronautics and Space Administration., eds. Timing the Geminga pulsar with high-energy gamma-rays: Final technical report for NAG5-2051. [Washington, DC?]: National Aeronautics and Space Administration, Compton Gamma-Ray Observatory, 1997.

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Book chapters on the topic "Pulsar timing"

1

Backer, D. C. "Pulsar Timing." In Timing Neutron Stars, 3–16. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_1.

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Taylor, Stephen R. "Pulsar Timing." In Nanohertz Gravitational Wave Astronomy, 35–52. Boca Raton: CRC Press, 2021. http://dx.doi.org/10.1201/9781003240648-3.

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Romani, Roger W. "Timing a Millisecond Pulsar Array." In Timing Neutron Stars, 113–17. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_6.

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Cheng, K. S., M. A. Alpar, D. Pines, and J. Shaham. "A Model of Pulsar Timing Noise." In Timing Neutron Stars, 503–9. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_45.

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Herold, H., T. Ertl, B. Finkbeiner, and H. Ruder. "Self-Consistent Modelling of Pulsar Magnetospheres." In Timing Neutron Stars, 723–29. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_56.

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Fruchter, A. S., D. R. Stinebring, and J. H. Taylor. "A Millisecond Pulsar in an Eclipsing Binary." In Timing Neutron Stars, 163–68. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_13.

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Smith, F. Graham. "Slowdown Rate and Oscillations in the Crab Pulsar." In Timing Neutron Stars, 153–56. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_11.

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Foster, Roger S., and James M. Cordes. "Simulation of Interstellar Scattering Effects on Pulsar Timing." In Timing Neutron Stars, 125–29. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_8.

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Mastichiadis, Apostolos. "X-Rays from a Possible Pulsar in Supernova 1987A." In Timing Neutron Stars, 305–15. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_26.

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Smith, F. Graham. "The Origin of High-Energy Radiation from the Crab Pulsar." In Timing Neutron Stars, 389–92. Dordrecht: Springer Netherlands, 1989. http://dx.doi.org/10.1007/978-94-009-2273-0_37.

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Conference papers on the topic "Pulsar timing"

1

Lazaridis, Kosmas. "Pulsar timing arrays." In From Antikythera to the Square Kilometre Array: Lessons from the Ancients. Trieste, Italy: Sissa Medialab, 2013. http://dx.doi.org/10.22323/1.170.0032.

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Janssen, G. H., B. W. Stappers, M. Kramer, M. Purver, A. Jessner, I. Cognard, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "European Pulsar Timing Array." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900317.

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Purver, Mark. "The European Pulsar Timing Array." In From Planets to Dark Energy: the Modern Radio Universe. Trieste, Italy: Sissa Medialab, 2008. http://dx.doi.org/10.22323/1.052.0125.

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Smits, Roy J. M. "The European Pulsar Timing Array." In ISKAF2010 Science Meeting. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.112.0080.

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Taylor, Joseph H. "Pulsar timing and relativisitic gravity." In Atomic physics 12. AIP, 1991. http://dx.doi.org/10.1063/1.40996.

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Manchester, R. N., C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "The Parkes Pulsar Timing Array Project." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900303.

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Paul, Ashis, Krishnakumar M.A., Lankeswar Dey, Manjari Bagchi, Mayuresh Surnis, Neelam Dhanda, P. K. Manoharan, et al. "The Indian Pulsar Timing Array (InPTA)." In 2019 URSI Asia-Pacific Radio Science Conference (AP-RASC). IEEE, 2019. http://dx.doi.org/10.23919/ursiap-rasc.2019.8738505.

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Manchester, R. N., Marta Burgay, Nicolò D’Amico, Paolo Esposito, Alberto Pellizzoni, and Andrea Possenti. "Pulsar Timing Arrays and their Applications." In RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE. AIP, 2011. http://dx.doi.org/10.1063/1.3615080.

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Ray, Paul S., Matthew Kerr, Damien Parent, Marta Burgay, Nicolò D’Amico, Paolo Esposito, Alberto Pellizzoni, and Andrea Possenti. "Pulsar Timing with the Fermi LAT." In RADIO PULSARS: AN ASTROPHYSICAL KEY TO UNLOCK THE SECRETS OF THE UNIVERSE. AIP, 2011. http://dx.doi.org/10.1063/1.3615094.

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Qiu, Wei, He Yin, Weikang Wang, Yilu Liu, Wenxuan Yao, Liangwei Zhan, Peter Fuhr, and Thomas King. "Pulsar Based Timing for Grid Synchronization." In 2020 IEEE Industry Applications Society Annual Meeting. IEEE, 2020. http://dx.doi.org/10.1109/ias44978.2020.9334812.

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Reports on the topic "Pulsar timing"

1

Duncan, M. G. Precision pulse-timing instrumentation for ultrasonic nondestructive testing. Office of Scientific and Technical Information (OSTI), August 1990. http://dx.doi.org/10.2172/6762029.

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