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Academic literature on the topic 'Pulsar observations'

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Published: 4 June 2021
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Journal articles on the topic "Pulsar observations"

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Wang, P. F., J. L. Han, L. Han, B. Y. Cai, C. Wang, T. Wang, X. Chen, et al. "Jiamusi pulsar observations." Astronomy & Astrophysics 644 (December 2020): A73. http://dx.doi.org/10.1051/0004-6361/202038867.

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Aims. Most pulsar nulling observations have been conducted at frequencies lower than 1400 MHz. We aim to understand the nulling behaviors of pulsars at relatively high frequencies, and to decipher whether or not nulling is caused by a global change in the pulsar magnetosphere. Methods. We used the Jiamusi 66 m telescope to observe 20 bright pulsars at 2250 MHz with unprecedented lengths of time. We estimated the nulling fractions of these pulsars, and identified the null and emission states of the pulses. We also calculated the nulling degrees and scales of the emission-null pairs to describe the distributions of emission and null lengths. Results. Three pulsars, PSRs J0248+6021, J0543+2329, and J1844+00, are found to null for the first time. The details of null-to-emission and emission-to-null transitions within the pulse window are observed for the first time for PSR J1509+5531, which is a low-probability event. A complete cycle of long nulls with timescales of hours is observed for PSR J1709−1640. For most of these pulsars, the K-S tests of nulling degrees and nulling scales reject the hypothesis that null and emission are caused by random processes at high significance levels. Emission-null sequences of some pulsars exhibit quasi-periodic, low-frequency or featureless modulations, which might be related to different origins. During transitions between emission and null states, pulse intensities have diverse tendencies for variation. Significant correlations are found between respectively nulling fraction, nulling cadence, and nulling scale and the energy loss rate of the pulsars. Combined with the nulling fractions reported in the literature for 146 nulling pulsars, we find that statistically large nulling fractions are more tightly related to pulsar period than to characteristic age or energy-loss rate.
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Wang, Na, R. N. Manchester, Aili Yusup, Xinji Wu, Jin Zhang, and Maozheng Chen. "Scintillation Observations of Strong Northern Pulsars." International Astronomical Union Colloquium 182 (2001): 57–60. http://dx.doi.org/10.1017/s0252921100000695.

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AbstractScintillation of pulsar radio emission provides information about the interstellar medium along the path to the pulsar and the velocities of pulsars. It also affects the precision of pulse timing observations. Using a pulsar timing system developed at the Urumqi Astronomical Observatory 25 m telescope, we observed diffractive scintillation dynamic spectra for several strong northern pulsars. This paper introduces the observing system and discusses the observational results.
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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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Edelstein, Jerry, and Stuart Bowyer. "EUV Observations of Pulsars." International Astronomical Union Colloquium 160 (1996): 291–95. http://dx.doi.org/10.1017/s0252921100041749.

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AbstractThree pulsars have been detected with the Lexan (100 Å )filter of the EUVE Deep Survey telescope: the middle-aged isolated pulsars, PSR B0656+14 and Geminga, plus the aged millisecond pulsar PSR J0437–4715. The EUV detections have been used both alone and in combination with observations in other bandpasses to limit the physical state of the objects and to test theories regarding neutron star cooling and re-heating mechanisms. For Geminga, the EUVE data suggests the presence of an optical cyclotron spectral feature superimposed on the Rayleigh-Jeans continuum tail from a hot pulsar surface. We summarize EUV pulsar observations and results.
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Torne, Pablo. "Pulsar observations at millimetre wavelengths." Proceedings of the International Astronomical Union 13, S337 (September 2017): 92–95. http://dx.doi.org/10.1017/s1743921317009085.

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AbstractDetecting and studying pulsars above a few GHz in the radio band is challenging due to the typical faintness of pulsar radio emission, their steep spectra, and the lack of observatories with sufficient sensitivity operating at high frequency ranges. Despite the difficulty, the observations of pulsars at high radio frequencies are valuable because they can help us to understand the radio emission process, complete a census of the Galactic pulsar population, and possibly discover the elusive population in the Galactic Centre, where low-frequency observations have problems due to the strong scattering. During the decades of the 1990s and 2000s, the availability of sensitive instrumentation allowed for the detection of a small sample of pulsars above 10 GHz, and for the first time in the millimetre band. Recently, new attempts between 3 and 1 mm (≈86 − 300 GHz) have resulted in the detections of a pulsar and a magnetar up to the highest radio frequencies to date, reaching 291 GHz (1.03 mm). The efforts continue, and the advent of new or upgraded millimetre facilities like the IRAM 30-m, NOEMA, the LMT, and ALMA, warrants a new era of high-sensitivity millimetre pulsar astronomy in the upcoming years.
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Wang, Na, Jin Zhang, and Xin-Ji Wu. "Pulsar Observations in China – Status and Results." Symposium - International Astronomical Union 214 (2003): 159–62. http://dx.doi.org/10.1017/s007418090019432x.

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We present the status and results of pulsar observations in China. Pulsar observations at Urumqi Observatory over more than two years have resulted in updated rotation parameters for 74 pulsars. Comparison with earlier observations shows that long-term period and period-derivative fluctuations are probably dominated by unseen glitches. We also monitored the variation of pulsar scintillation dynamic spectra for a few strong pulsars. The data show major variations in the scintillation parameters. A new system at a lower frequency is planned to allow investigation of the frequency dependence of pulsar properties. A 50-m telescope for millisecond pulsar timing is also being planned at the National Astronomical Observatories, Beijing, and should be constructed within three years.
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McCulloch, P. M. "Closing Comments: Observations." International Astronomical Union Colloquium 128 (1992): 410–11. http://dx.doi.org/10.1017/s0002731600155659.

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During the course of this colloquium many papers have been presented on observational aspects of pulsar astronomy. In the following discussion I have not attempted to be comprehensive but have selected a number of areas of interest to me.The basic pulsar properties appear to be consistent over the full range of pulsar periods from 1 ms to 4s, implying that the emission mechanism is the same for all pulsars. There was a general consensus among the observers that the radio emission occurs low down in the pulsar's magnetosphere above the magnetic polar region.
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Collins, Susan, Andy Shearer, Ben Stappers, Cesare Barbieri, Giampiero Naletto, Luca Zampieri, Enrico Verroi, and Serena Gradari. "Crab Pulsar: Enhanced Optical Emission During Giant Radio Pulses." Proceedings of the International Astronomical Union 7, S285 (September 2011): 296–98. http://dx.doi.org/10.1017/s1743921312000841.

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AbstractAlthough optical pulsar studies have been limited to a few favoured objects, the observation of pulsars at optical wavelengths provides an opportunity to derive a number of important pulsar characteristics, including the energy spectrum of the emitting electrons and the geometry of the emission zone. These parameters will be vital for a comprehensive model of pulsar emission mechanisms. Observations of the Crab pulsar with the high-time-resolution photon-tagging photometer IquEYE show an optical–radio delay of ~178 μs. Incorporating simultaneous Jodrell Bank radio observations suggested a correlation between giant radio pulses and enhanced optical pulses for this pulsar, thus offering possible evidence for the reprocessing of radio photons.
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Kawai, Nobuyuki, and Keisuke Tamura. "Recent X-ray Observations of Pulsar Nebulae." International Astronomical Union Colloquium 160 (1996): 367–74. http://dx.doi.org/10.1017/s0252921100041920.

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AbstractResults from the X-ray observations of pulsars with ASCA are presented. The surroundings of pulsars are investigated in detail taking advantage of ASCA’s unique capabilities; high spectral resolution and a high throughput over a wide energy range from 0.4 keV to 10 keV. The spectral characteristics of the nebulae of PSR B1509—58 and the Vela pulsar are spectroscopically investigated. A jet-like feature is found from PSR B1509—58. We detected diffuse emission sources in the vicinity of many pulsars. The high probability of finding such diffuse sources for many pulsars suggests that they exist universally for all the active pulsars, and that they are powered by the pulsars. SNR Kes 32 was imaged in X-ray for the first time. Its X-ray properties can be used to examine its association with the nearby pulsar PSR B1610—50.
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Navarro, José, and R. N. Manchester. "Polarimetric Observations of PSR J0437–4715." International Astronomical Union Colloquium 160 (1996): 249–51. http://dx.doi.org/10.1017/s0252921100041622.

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To date there have been few polarimetric observations of millisecond pulsars, mainly due to the instrumental challenge of simultaneous high time resolution and large bandwidth. Such observations provide our most direct clues to the structure of the magnetic fields around pulsars, and are especially important in the case of millisecond pulsars, where radio emission necessarily originates very close to the neutron star surface.We have observed the bright millisecond pulsar J0437–4715 at the Parkes Radiotelescope with the Caltech Fast Pulsar Timing Machine, at several radio frequencies and in full polarimetric mode. Our analyses show significant deviations from the standard dipole field geometry.
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Dissertations / Theses on the topic "Pulsar observations"

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Martín, Rodríguez Jonatan. "Theory & observations of the PWN-SNR complex." Doctoral thesis, Universitat Autònoma de Barcelona, 2014. http://hdl.handle.net/10803/283894.

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In this work, we study theoretical and observational issues about pulsars (PSRs), pulsar wind nebulae (PWNe) and supernova remnants (SNRs). In particular, the spectral modeling of young PWNe and the X-ray analysis of SNRs with magnetars comparing their characteristics with those remnants surrounding canonical pulsars. The spectra of PWNe range from radio to γ-rays. They are the largest class of identified Galactic in γ-rays increasing the number from 1 to ∼30 during the last years. We have developed a detailed spectral code which reproduces the electromagnetic spectrum of PWNe in free expansion (tage .10 kyr). We shed light and try to understand issues on time evolution of the spectra, the synchrotron self-Compton dominance in the Crab Nebula, the particle dominance in PWNe detected at TeV energies and how physical parameters constrain the detectability of PWNe at TeV. We make a systematic study of all Galactic, TeV-detected, young PWNe which allows to find correlations and trends between parameters. We also discuss about the spectrum of those PWNe not detected at TeV and if models with low magnetized nebulae can explain the lack of detection or, on the contrary, high-magnetization models are more favorable. Regarding the X-ray analysis of SNRs, we use X-ray spectroscopy in SNRs with magnetars to discuss about the formation mechanism of such extremely magnetized PSRs. The alpha-dynamo mechanism proposed in the 1990’s produces an energy release that should have influence in the energy of the SN explosion. We extend the work done previously done by Vink & Kuiper (2006) about the energetics of the SN explosion looking for this energy release and we look for the element ionization and the X-ray luminosity and we compare our results with other SNRs with an associated central source.
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Çelik, Özlem. "Observations of crab nebula and pulsar with VERITAS." Diss., Restricted to subscribing institutions, 2008. http://proquest.umi.com/pqdweb?did=1781954321&sid=2&Fmt=2&clientId=1564&RQT=309&VName=PQD.

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Ibrahim, Abubakr. "Dispersion measure variations in pulsar observations with LOFAR." Master's thesis, Faculty of Science, 2019. https://hdl.handle.net/11427/31609.

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I present an analysis of the dispersion measure (DM) variations for 68 pulsars. The observations were taken using six International LOFAR Stations in Europe over the period of 3.5 years (between June 2014 and November 2017) at the centre frequency of 150 MHz with 80 MHz of bandwidth. During this time each pulsar was observed on weekly basis resulting in an average of 160 observations per source. I show that, the variations of the DM measurements show various trends along the span of the observation: increasing or decreasing, and in some cases more changes from one trend to another. I perform the structure function analysis for each of observed pulsar included in the study, in order to check if the DM variations follow the Kolmogorov power spectrum which describes the turbulence structure of the interstellar medium (ISM). I find that for a number of pulsars results show consistency with the Kolmogorov distribution (e.g. PSRs J1913−0440 and J2157+4017) while other sources show significant difference (e.g. PSRs J0108+6608 and J0614+2229). I also obtain the DM derivatives (i.e. dDM/dt) for each pulsar, in order to examine the correlation between the DM and its derivative. The result of this correlation shows a best-fit with a square-root dependence of 0.6±0.2, which is comparable with the result that was previously obtained by Hobbs et al. (2004), who shows a dependence of square-root between the DM and its derivative; with a gradient of 0.57±0.09. Also, one of the major results of this study that, thanks to the timing analysis, allowed me to produce a new timing solution for three pulsars: PSRs J0613+3731, J0815+4611 and J1740+27. This study concludes in that: i) the DM variations can be used to understand the general properties of the ISM ii) the low-frequency observations can enable us to study the dispersion effect on pulsar signals, which can be very useful for the effort of the pulsar timing array (PTA) project iii) IISM studies using pulsar timing is a powerful technique requiring careful approach to data reduction and analysis due to characteristic of the pulsars.
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Lin, Tingting. "Pulsar Wind Nebulae: observations and models of 3C58 and discovery of superefficiency." Doctoral thesis, Universitat Autònoma de Barcelona, 2020. http://hdl.handle.net/10803/671177.

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Aquesta tesi està centrada en l’estudi de les nebuloses produïdes pel vent dels pulsars (acrònim anglès, PWNe), que es formen com a resultat de que la major part de l’energia rotacional del púlsar es perd per l’emissió d’un vent relativista de partícules. Els vents, supersònics respecte al medi interestel·lar, produeixen un xoc terminal on les partícules s’acceleren. Atès que la nebulosa conté fotons i camps magnètics, les partícules poden emetre a totes les freqüències, des de ràdio fins a energies TeV, mitjançant processos no tèrmics com el sincrotró i el Compton invers. Aquesta tesi estudia l’evolució d’aquesta radiació no tèrmica al llarg de la vida del púlsar, analitzant els canvis produïts a la distribució d’energia espectral com a resultat de l’expansió i la contracció del PWN a causa dels equilibris de pressió i la interacció amb l’entorn. La tesi considera en primer lloc el cas del complex format pel púlsar/PWN, PSR J0205 + 6449/3C 58, que és especial per la seva curta edat, la seva significativa potència i la seva similitud amb la nebulosa del Cranc (la millor estudiada). Es presenten els resultats de l’anàlisi de 8 anys de dades de Fermi-LAT. Utilitzant una efemèride contemporània per a la pulsació, s’ha pogut detectar significativament 3C 58 durant l’interval de fase fora del pic de PSR J0205 + 6449. He analitzat les dades amb un model de PWNe en funció del temps basat en el codi TIDE, desenvolupat pel grup en el que he treballat durant els darrers 8 anys. El meu model proporciona un ajust raonable a les dades; un en el que el PWN 3C 58 encara no reverbera. La reverberació és el període de l’evolució de les nebuloses quan el xoc invers creat per l’explosió de la supernova viatja cap al púlsar, comprimint-les. És un període relativament curt, però significatiu i que no ha estat gaire estudiat. La resta de la tesi estudia PWNe més antigues, o més joves com 3C 58, però evolucionant-les cap al futur per a analitzar el seu comportament durant la reverberació. Aquest estudi ha conduït al descobriment i caracterització de la supereficiència. La supereficiència succeeix quan, a causa de la seva compressió deguda al xoc invers que torna de l’explosió de la supernova, la nebulosa està sotmesa a un escalfament adiabàtic significatiu. Degut a la compressió, el camp magnètic de la PWN també augmenta, així com hi ha més partícules a energies més altes que les que hi havia abans. Vaig trobar que aquest procés pot produir PWNe que durant poc temps emeten més energia en raigs X i en altres freqüències que el que tenen com a energia de rotació en aquell moment. Aquesta aparent contradicció és conseqüència del fet que potència rotacional del púlsar ja no és el dipòsit d’energia del sistema. Aquest període finalitza quan la pressió del camp magnètic, que augmenta significativament, és capaç d’equilibrar la pressió cinemàtica proporcionada pel xoc invers. He estudiat tant PWNe ben caracteritzades com una àmplia gamma de models de PWN representatius dels púlsars observats per estudiar les seves propietats de reverberació i supereficiència. Finalment, he estimat, mitjançant simulacions de Monte Carlo, quantes PWNe galàctics s’espera que reverberin o estiguin en una etapa de supereficiència en un moment donat i he realitzat prediccions per a possibles deteccions futures amb la propera generació d’instruments. Aquesta tesi es presenta com un compendi de resultats publicats. Tres articles publicats a The Astrophysical Journal, The Astrophysical Journal Letters i Monthly Notices of the Royal Astronomical Society conformen els capítols 2, 3 i 4 de la tesi.
Esta tesis se centra en el estudio de las nebulosas producidas por los vientos de púlsares (de su acrónimo en inglés, PWNe), que se forman como resultado de que la mayor parte de la energía de rotación del púlsar se pierde a través de la emisión de un viento relativista de partículas. Los vientos, al ser supersónicos con respecto al medio interestelar, producen un choque terminal donde las partículas se aceleran. Dado que la nebulosa contiene campos magnéticos y de fotones, las partículas pueden emitir en todas las frecuencias, desde radio hasta las energías TeV, a través de procesos no térmicos como sincrotrón y Compton inverso. Esta tesis estudia la evolución de esta radiación no térmica a lo largo de la vida del púlsar, analizando los cambios producidos en la distribución espectral de energía como resultado de la expansión y contracción del PWN debido a los equilibrios de presión y la interacción con el entorno. La tesis primero considera el caso del complejo formado por el púlsar/PWN, PSR J0205 + 6449/3C 58, que es especial por su corta edad, significativa potencia y parecido con la Nebulosa del Cangrejo (la mejor estudiada). Se presentan los resultados del análisis de 8 años de datos de Fermi-LAT. Utilizando una efeméride contemporánea para la pulsación, se ha podido detectar significativamente 3C 58 durante el intervalo de fase fuera del pico de PSR J0205 + 6449. He analizado estos datos con un modelo de PWNe dependiente del tiempo basado en el código TIDE, desarrollado por el grupo en el que he trabajado durante los últimos 8 años. Mi modelo proporciona un ajuste razonable a los datos; uno en el que el PWN 3C 58 aún no está en reverberación. La reverberación es el período de evolución de las nebulosas que ocurre cuando el choque inverso creado por la explosión de la supernova viaja hacia el púlsar, comprimiéndolas. Es un período relativamente corto pero significativo y apenas estudiado. El resto de tesis estudia PWNe más viejas, o más jóvenes como 3C 58 pero evolucionándolas hacia el futuro para analizar el comportamiento que muestran durante reverberación. Este estudio ha llevado al descubrimiento y caracterización de la supereficiencia. La supereficiencia ocurre cuando, debido a su compresión debido al impacto del choque inverso de la explosión de la supernova, la nebulosa está sujeta a un calentamiento adiabático significativo. Debido a la compresión, el campo magnético del PWN también aumenta, así como también hay más partículas a energías más altas que antes. Descubrí que tal proceso puede producir PWNe que durante un corto tiempo emiten más rayos X y fotones a otras frecuencias de lo que existe como energía de rotación en ese momento. Esto es consecuencia de que la potencia rotacional del púlsar ya no es la reserva de energía del sistema. Este período de reverberación termina cuando la presión del campo magnético, aumentada debido al incremento del propio campo, es capaz de equilibrar la presión cinemática proporcionada por el choque inverso. He estudiado tanto varias PWNe bien caracterizadas como una amplia gama de modelos PWN representativos de los púlsares observados para estudiar sus propiedades de reverberación y supereficiencia. Finalmente, estimé a través de simulaciones de Monte Carlo cuántas PWNe galácticas se espera que estén reverberando o en una etapa de supereficiencia en un momento dado y realicé predicciones para posibles detecciones futuras con la próxima generación de instrumentos. Esta tesis se presenta como un compendio de resultados publicados. Tres artículos publicados en The Astrophysical Journal, The Astrophysical Journal Letters y Monthly Notices of the Royal Astronomical Society conforman correspondientemente los Capítulos 2, 3 y 4 de la tesis.
This thesis focuses on the study of Pulsar wind Nebulae (PWNe), which form as a result of the bulk of the pulsar rotational energy begin lost via the emission of a relativistic wind of particles. The winds, being supersonic with respect to the interstellar medium, produce a termination shock where particles are accelerated. Since the nebula is threaded with photon and magnetic fields, particles are able to emit at all frequencies, from radio to TeV energies, via non-thermal processes such as synchrotron and inverse Compton. This thesis zooms into studying the evolution of this non-thermal radiation along the pulsar lifetime, analyzing the changes produced to the spectral energy distribution as a result of the expansion and contraction of the PWN due to pressure balances and interaction with the environment. The thesis first considers the case of the complex formed by the pulsar/PWN, PSR J0205+6449/3C 58, which is especial due to its young age, significant power, and similarity to the Crab Nebula (the best studied PWN). The thesis presents the results of the analysis of 8 years of Fermi-LAT data. The main aspect is that using a contemporaneous ephemeris for the pulsation, we could significantly detect 3C 58 during the off-peak phase interval of PSR J0205+6449. I analyzed the observed data with a time-dependent model of PWNe based on the code TIDE, developed by the group in which I worked over the last 8 years. My model provides a reasonable fit to data; one in which the PWN 3C 58 is not yet reverberating. Reverberation is the period of PWN evolution when the reverse shock created by the supernova explosion travels back towards the pulsar, compressing the wind bubble. It is a relatively short but significant period, barely studied. The rest of the thesis studies older PWNe, or younger ones like 3C 58 but evolved into the future so as to grasp the behavior of reverberation when they pass through it. This study has led to the discovery and characterization of superefficiency. Superefficiency happens when, due to its compression because of the returning reverse shock of the supernova explosion, the nebula is subject to significant adiabatic heating. To what extent this heating affected the luminosities of the PWN at different energy ranges was not clear. The thesis describes in detail how due to the compression, the magnetic field of the PWN also increases, as well as there are more particles at higher energies than there were previously. I found that such process can produce PWNe that for a short time emit more in X-rays and other frequencies than what they have as rotational energy at the time. The former is not a paradox, but the consequence of the fact that the rotational spinning down of the pulsar is no longer the energy reservoir of the system. This period ends when the magnetic field pressure, increased because of the magnetic field, significantly risen up, is able to detain the kinematic pressure provided by the reverse shock. I took on both, several well-characterized PWNe and a broad range of PWN models representative of the observed pulsars to study their reverberation and superefficiency properties. Having attained such modelling, I estimated via Monte Carlo simulations how many Galactic PWNe are expected to be reverberating or in a superefficiency stage at any given time and realized predictions for possible future detections with the next generation of instruments. This thesis is presented as a compendium of published results. Three papers published in The Astrophysical Journal, The Astrophysical Journal Letters, and Monthly Notices of the Royal Astronomical Society correspondingly conform Chapters 2, 3 and 4 of the thesis.
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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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Fairhead, Laurent. "Chronométrage du pulsar milliseconde PSR1937+214 : analyse astrométrique et observations à Nançay." Observatoire de Paris, 1989. https://hal.archives-ouvertes.fr/tel-02149841.

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Les données de haute précision de chronométrage des pulsars rapides vont contribuer significativement à l'astrophysique des étoiles à neutrons, à la dynamique du système solaire, à l'astrométrie, à la métrologie du temps et à la cosmologie. Deux années de données de chronométrage du pulsar rapide PSR1937+214 ont été analysées afin de déterminer d'éventuelles erreurs systématiques introduites par les modèles d'analyse. Un logiciel d'analyse a été développé à cette fin. Des erreurs systématiques bien supérieures aux incertitudes théoriques calculées ont ainsi été révélées. Les paramètres du pulsar déterminés par la procédure d'analyse, comme sa période et sa position, dépendent alors fortement des théories du mouvement de la Terre et des échelles de temps utilisées dans l'analyse. D’autre part, des observations de chronométrage de pulsars rapides ont débuté à l'Observatoire de Nançay. Celles-ci nécessitent un dispositif spécial afin de compenser l'effet de dispersion de la matière ionisée interstellaire. Le dispositif adopte et construit à Nançay à cet effet est décrit ainsi que les programmes permettant son fonctionnement. Les méthodes d'observation et les résultats préliminaires d'une campagne d'observation effectuée au cours de l'été 1988 sont donnés.
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Carstairs, Ian Ruthven. "Kernel density estimators applied to hard X-ray observations of the Crab Pulsar." Thesis, University of Southampton, 1992. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.315292.

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Tsurusaki, Kazuma. "VERITAS observations of galactic gamma-ray sources." Diss., University of Iowa, 2012. https://ir.uiowa.edu/etd/3394.

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The main topic of this thesis is analysis of an unidentified Galactic TeV gamma-ray source, MGRO J1908+06, discovered by Milagro instrument in 2007. We analyzed 54 hours of observational data from the Very Energetic Radiation Imaging Telescope Array System (VERITAS), a ground-based gamma-ray observatory in southern Arizona comprised of an array of four Cherenkov Telescopes that reconstructs the energy and direction of astrophysical gamma-rays by imaging Cherenkov light emitted by energetic particles in air showers produced by the primary gamma-rays. MGRO J1908+06 is located between a supernova remnant SNR G40.5-0.5 and a young, energetic pulsar PSR J1907+0602. We studied the energy dependent morphology of the TeV emission from the source and measured the source extent and spectrum. The source extends well past the boundary of the SNR and is not correlated with strong radio continuum or molecular line emission which likely excludes an origin for the emission as solely due to the SNR. While emission in the 0.5-1.25 TeV band was centered around the pulsar, higher energy emission was observed near the supernova remnant. This morphology is opposite that observed in other pulsar wind nebulae. We proposed two models for the high energy emission located well away from the pulsar but close to the SNR: (1) shock acceleration at the shock front created by an interaction between the pulsar wind and the dense gas at the edge of the SNR or (2) molecular clouds around the SNR provides seed photons with energies higher than those from Cosmic Microwave Backgrounds for inverse Compton scattering. The former model can be tested by looking for molecular emission lines that trace shocks and by measuring the pulsar velocity. In addition, we investigated the gamma-ray emission from the nova explosion of V407 Cygni that occurred in March 2010. The Fermi-LAT observed this event in the energy range of E >100 MeV. The origins of the gamma-ray emission that the Fermi-LAT team proposed are either protons (hadronic model) or electrons (leptonic model), both of which were accelerated at the nova shock via the Fermi acceleration mechanism. We did not consider their leptonic model because no TeV gamma-ray emission is predicted. Their hadronic model can generate TeV gamma-rays with the modeled parameters. We found no evidence for TeV emission. We showed that with the flux upper limit calculated using the VERITAS data imposes constraints on the extension of the proton spectrum at high energies.
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Matheson, Heather. "X-ray observations of the young pulsar wind nebula G21.5–0.9 and the evolved pulsar wind nebulae CTB 87 (G74.9+1.2) and G63.7+1.1." IOP Publishing Ltd. for The American Astronomical Society, 2010. http://hdl.handle.net/1993/30163.

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Pulsar wind nebulae (PWNe), nebulae harbouring a rotation-powered neutron star that was born in a supernova, provide opportunities to study highly relativistic pulsar winds and their interaction with the surrounding medium. Particularly interesting are PWNe that do not show any sign of the expected surrounding SNR shell and were thought to be born in subenergetic explosions or with unusual progenitors. The detection of a shell around one such PWN suggested that shells are indeed produced but may be faint due to unseen shocked ejecta, a low density environment, and/or a young age that has not yet allowed the shell to brighten and become visible. Here, by using observational X-ray data from modern telescopes with excellent spatial and energy resolution (Chandra and XMM-Newton), we target PWNe that do not have prominent SNR shells, and are known to be in varied environments, to further explore the characteristics of this growing, but poorly explored, class of PWNe. By combining imaging and spectroscopic results, we study the morphology of the PWNe, search for thermal emission from shock-heated material, investigate the energetics of the nebulae, and search for candidates for the neutron stars powering the nebulae. We find that while the faint shell surrounding G21.5–0.9 can be explained as a young PWN evolving in a low density medium, CTB 87 (G74.9+1.2) appears to be in an advanced stage of evolution, and G63.7+1.1 appears to be both in an advanced stage of evolution and in a dense environment. By performing spatially resolved spectroscopy, we have shown how the spectral characteristics vary across the PWNe, and note that more data will place better constraints on possible thermal emission in these remnants. The imaging portion of these studies has revealed intriguing large-scale morphologies for CTB 87 and G63.7+1.1, as well as a torus-jet structure in CTB 87 and neutron star candidates in both CTB 87 and G63.7+1.1. We conclude that both CTB 87 and G63.7+1.1 are likely interacting with the supernova remnant reverse shock, and CTB 87 may be additionally influenced by the motion of its neutron star.
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Wilcox, Patrick Dean. "Observations of supernova remnants at very high energies with VERITAS." Diss., University of Iowa, 2019. https://ir.uiowa.edu/etd/7045.

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The constant flux of cosmic rays that bombard Earth from within our own galaxy are understood to come from both shell-type supernova remnants and pulsar wind nebulae (PWNe). Multiwavelength study of these objects can help us to understand what types of particles are accelerated, and gamma-ray emission is key to understanding the highest energy cosmic rays. In this thesis, I analyze and interpret observations made with the Very Energetic Radiation Imaging Telescope Array System (VERITAS), a gamma-ray telescope located in Southern Arizona. LS 5039 and HESS J1825-137 occupy the same field of view on the sky and were observed for about 8 hours with VERITAS. LS 5039 is a gamma-ray binary, and the observations supports theories that the compact object hosts a PWN which is continuously interacting with the nearby star. HESS J1825-137 is a very extended PWN with an extent of diameter greater than 1 degree on the sky. Using the VERITAS observations, I am able to measure the radial profile and compare the gamma-ray luminosity to other PWN. DA 495, a "Crab-like" PWN with unusually strong magnetic fields, was observed for about 70 hours with VERITAS. In this study, results are combined with radio and X-ray spectral information to allow for detailed astrophysical modeling of the region. This broadband spectral modeling places constraints on the properties of the particle population in this PWN and allows for both leptonic and hadronic emission scenarios to be evaluated. Hadronic scenarios instil doubt on the pure PWN interpretation and favor a previously undetected shell-type remnant being present.
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Books on the topic "Pulsar observations"

1

López Coto, Rubén. Very-high-energy Gamma-ray Observations of Pulsar Wind Nebulae and Cataclysmic Variable Stars with MAGIC and Development of Trigger Systems for IACTs. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-44751-3.

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Frail, Dale A. A study of the diffuse interstellar medium through neutral hydrogen absorption observations toward pulsars. Toronto: University of Toronto, Dept. of Astronomy, 1989.

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EGRET observations of the Vela pulsar, PSR 0833-45. Garching, Germany: Max-Planck-Institut fur Extraterrestrische Physik, 1994.

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G, Kanbach, and United States. National Aeronautics and Space Administration., eds. EGRET observations of the Vela pulsar, PSR 0833-45. Garching, Germany: Max-Planck-Institut fur Extraterrestrische Physik, 1994.

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United States. National Aeronautics and Space Administration., ed. [ROSAT observations of the binary BE-star/radio pulsar PSR1259-6]: [semiannual technical report, 15 Jan. - 1 Aug. 1993]. [Washington, DC: National Aeronautics and Space Administration, 1993.

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[ROSAT observations of the binary BE-star/radio pulsar PSR1259-6]: [semiannual technical report, 15 Jan. - 1 Aug. 1993]. [Washington, DC: National Aeronautics and Space Administration, 1993.

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R, Cominsky Lynn, and United States. National Aeronautics and Space Administration., eds. ROSAT observations of the binary Be-star/radio pulsar PSR1259-63: Final technical report for NASA NAG 5-1684. [Washington, DC: National Aeronautics and Space Administration, 1994.

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ROSAT observations of the binary Be-star/radio pulsar PSR1259-63: Final technical report for NASA NAG 5-1684. [Washington, DC: National Aeronautics and Space Administration, 1994.

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Coto, Rubén López. Very-high-energy Gamma-ray Observations of Pulsar Wind Nebulae and Cataclysmic Variable Stars with MAGIC and Development of Trigger Systems for IACTs. Springer, 2018.

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Maggiore, Michele. Neutron stars. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198570899.003.0002.

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Observation of neutron stars as pulsars. Pulsar demography. Magnetars. GW emission from neutron stars. Normal modes of neuton stars. CFS instability; r-mode instability. GWs from the post-merger NS remnant. Ellipticity of deformed neutron stars.
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Book chapters on the topic "Pulsar observations"

1

Temim, Tea, and Patrick Slane. "Optical and Infrared Observations of Pulsar Wind Nebulae." In Modelling Pulsar Wind Nebulae, 29–46. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-63031-1_2.

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de Jager, Ocker C., and Arache Djannati-Ataï. "Implications of HESS Observations of Pulsar." In Neutron Stars and Pulsars, 451–79. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76965-1_17.

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Slane, Patrick. "Multiwavelength Observations of Pulsar Wind Nebulae." In High-Energy Emission from Pulsars and their Systems, 373–91. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-17251-9_32.

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Queloz, D. "Indirect Searches: Doppler Spectroscopy and Pulsar Timing." In Planets Outside the Solar System: Theory and Observations, 229–48. Dordrecht: Springer Netherlands, 1999. http://dx.doi.org/10.1007/978-94-011-4623-4_15.

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Pedaletti, Giovanna. "Prospects for Pulsar Wind Nebulae Observations with γ-Ray Astronomy Facilities: Cherenkov Telescope Array and Satellites." In Modelling Pulsar Wind Nebulae, 81–100. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-63031-1_5.

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Ramesh bhat, N. D., Yashwant Gupta, and A. Pramesh Rao. "Pulsar Observations and Structure of the Local ISM." In Science with Minisat 01, 227–31. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0686-6_23.

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Stairs, Ingrid H., M. Kramer, R. N. Manchester, M. A. McLaughlin, A. G. Lyne, R. D. Ferdman, M. Burgay, et al. "Observations of the Double Pulsar PSR J0737–3039A/B." In Astrophysics and Space Science Library, 53–62. Dordrecht: Springer Netherlands, 2008. http://dx.doi.org/10.1007/978-1-4020-6544-6_3.

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Warwick, R. S., M. G. Watson, and R. Willingale. "Exosat Observations of the X-Ray Pulsar 4U1145-619." In X-Ray Astronomy in the Exosat Era, 429–32. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5448-9_60.

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López Coto, Rubén. "Introduction to Pulsar Wind Nebulae." In Very-high-energy Gamma-ray Observations of Pulsar Wind Nebulae and Cataclysmic Variable Stars with MAGIC and Development of Trigger Systems for IACTs, 107–26. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-44751-3_5.

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Sun, Hai-feng, Jian-yu Su, Liang Zhao, Zhi-wei Liu, and Hai-yan Fang. "Building the Crab Pulsar Timing Model with XPNAV-1 Observations." In Lecture Notes in Electrical Engineering, 897–907. Singapore: Springer Singapore, 2018. http://dx.doi.org/10.1007/978-981-13-0029-5_75.

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Conference papers on the topic "Pulsar observations"

1

Hessels, Jason, Ben Stappers, Anastasia Alexov, Thijs Coenen, Tom Hassall, Aris Karastergiou, Vladislav K. Kondratiev, et al. "Early Pulsar Observations with LOFAR." In ISKAF2010 Science Meeting. Trieste, Italy: Sissa Medialab, 2010. http://dx.doi.org/10.22323/1.112.0025.

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Germanà, C., L. Zampieri, I. Capraro, C. Facchinetti, G. Naletto, T. Occhipinti, E. Verroi, et al. "Crab Pulsar Observations with AquEYE." In SIMBOL-X: FOCUSING ON THE HARD X-RAY UNIVERSE: Proceedings of the 2nd International Simbol-X Symposium. AIP, 2009. http://dx.doi.org/10.1063/1.3149457.

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Strickman, M. S. "RXTE observations of the Vela Pulsar: The pulsar rosetta stone." In GAMMA 2001: Gamma-Ray Astrophysics 2001. AIP, 2001. http://dx.doi.org/10.1063/1.1419465.

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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." In COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44120.

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Rozko, Karolina, Wojciech Lewandowski, Jaroslaw Kijak, Andrzej Krankowski, Leszek Blaszkiewicz, Pawel Flisek, Krzysztof Chyzy, and Bartosz Smierciak. "Pulsar observations using the POLFAR stations." In 2020 Baltic URSI Symposium (URSI). IEEE, 2020. http://dx.doi.org/10.23919/ursi48707.2020.9254061.

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Zitzer, Benjamin, and VERITAS Collaboration. "VERITAS observations of the Crab pulsar." In HIGH ENERGY GAMMA-RAY ASTRONOMY: 5th International Meeting on High Energy Gamma-Ray Astronomy. AIP, 2012. http://dx.doi.org/10.1063/1.4772256.

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López, M., N. Otte, E. Aliu, W. Bednarek, J. L. Contreras, K. Hirotani, and M. Rissi. "Pulsar observations with the MAGIC Telescope." In THE FIRST GLAST SYMPOSIUM. AIP, 2007. http://dx.doi.org/10.1063/1.2757375.

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de Jager, Ocker C. "HESS Observations of Pulsar Wind Nebulae." In ASTROPHYSICAL SOURCES OF HIGH ENERGY PARTICLES AND RADIATION. AIP, 2005. http://dx.doi.org/10.1063/1.2141885.

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Nel, H. I., O. C. De Jager, L. J. Haasbroek, B. C. Raubenheimer, C. Brink, P. J. Meintjes, A. R. North, G. Van Urk, and B. Visser. "TeV observations of gamma-ray pulsar: A test for pulsar models." In COMPTON GAMMA-RAY OBSERVATORY. AIP, 1993. http://dx.doi.org/10.1063/1.44129.

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Joshi, Bhal Chandra, Arun Naidu, and P. K. Manoharan. "Upgrade of legacy ORT for pulsar observations." In 2019 URSI Asia-Pacific Radio Science Conference (AP-RASC). IEEE, 2019. http://dx.doi.org/10.23919/ursiap-rasc.2019.8738231.

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Reports on the topic "Pulsar observations"

1

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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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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Sadler, Brian M., and Stephen D. Casey. On Periodic Pulse Interval Analysis with Outliers and Missing Observations. Fort Belvoir, VA: Defense Technical Information Center, January 1996. http://dx.doi.org/10.21236/ada454910.

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Jacobson, A. R., and R. C. Carlos. Observations of prolonged ionospheric anomalies following passage of an infrasound pulse through the lower thermosphere. Office of Scientific and Technical Information (OSTI), June 1987. http://dx.doi.org/10.2172/6322972.

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Meyer, Perry A., Ellen BK Baer, Judith A. Bamberger, James A. Fort, and Michael J. Minette. Assessment of Differences in Phase 1 and Phase 2 Test Observations for Waste Treatment Plant Pulse Jet Mixer Tests with Non-Cohesive Solids. Office of Scientific and Technical Information (OSTI), October 2010. http://dx.doi.org/10.2172/992015.

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Coastal Lidar And Radar Imaging System (CLARIS) mobile terrestrial lidar survey along the Outer Banks, North Carolina in Currituck and Dare counties. Coastal and Hydraulics Laboratory (U.S.), January 2020. http://dx.doi.org/10.21079/11681/39419.

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The Coastal Observation and Analysis Branch (COAB) located at the Field Research Facility (FRF) conducts quarterly surveys and post-storm surveys along up to 60 kilometers of coastline within the vicinity of the FRF to assess, evaluate, and provide updated observations of the morphology of the foreshore and dune system. The surveys are conducted using a mobile terrestrial LiDAR scanner coupled with an Inertial Navigation System (INS). Traditionally the surveys coincide with a low tide, exposing the widest swath of visible sediment to the scanner as well as enough wind-sea swell or texture to induce wave breaking upon the interior sandbars. The wave field is measured with X-Band radar which records a spatial time series of wave direction and speed. Data for the survey region was collected using the VZ-2000's mobile, 3D scanning mode where the scanner continuously rotates the line scan 360 degrees as the vehicle progresses forward. Elevation measurements are acquired on all sides of the vehicle except for the topography directly underneath the vehicle. As the vehicle moves forward, the next rotation will capture the previous position's occluded data area. Laser data is acquired in mobile 3D radar mode with a pulse repetition rate of 300kHz, theta resolution of 0.19 degrees and phi resolution of 0.625 degrees. Horizontal Datum NAD83(2011), Projection North Carolina State Plane (3200) meters; Vertical Datum NAVD88, meters with geoid09 applied.
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Coastal Lidar And Radar Imaging System (CLARIS) mobile terrestrial lidar survey along the Outer Banks, North Carolina in Currituck and Dare counties. Coastal and Hydraulics Laboratory (U.S.), January 2020. http://dx.doi.org/10.21079/11681/39419.

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The Coastal Observation and Analysis Branch (COAB) located at the Field Research Facility (FRF) conducts quarterly surveys and post-storm surveys along up to 60 kilometers of coastline within the vicinity of the FRF to assess, evaluate, and provide updated observations of the morphology of the foreshore and dune system. The surveys are conducted using a mobile terrestrial LiDAR scanner coupled with an Inertial Navigation System (INS). Traditionally the surveys coincide with a low tide, exposing the widest swath of visible sediment to the scanner as well as enough wind-sea swell or texture to induce wave breaking upon the interior sandbars. The wave field is measured with X-Band radar which records a spatial time series of wave direction and speed. Data for the survey region was collected using the VZ-2000's mobile, 3D scanning mode where the scanner continuously rotates the line scan 360 degrees as the vehicle progresses forward. Elevation measurements are acquired on all sides of the vehicle except for the topography directly underneath the vehicle. As the vehicle moves forward, the next rotation will capture the previous position's occluded data area. Laser data is acquired in mobile 3D radar mode with a pulse repetition rate of 300kHz, theta resolution of 0.19 degrees and phi resolution of 0.625 degrees. Horizontal Datum NAD83(2011), Projection North Carolina State Plane (3200) meters; Vertical Datum NAVD88, meters with geoid09 applied.
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