Relevant bibliographies by topics / Pulsars – Observations

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  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
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Academic literature on the topic 'Pulsars – Observations'

Author: Grafiati
Published: 4 June 2021
Last updated: 21 December 2024

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Journal articles on the topic "Pulsars – Observations"

1

Balakrishnan, Vishnu, David Champion, Ewan Barr, Michael Kramer, V. Venkatraman Krishnan, Ralph P. Eatough, Rahul Sengar, and Matthew Bailes. "Coherent search for binary pulsars across all Five Keplerian parameters in radio observations using the template-bank algorithm." Monthly Notices of the Royal Astronomical Society 511, no. 1 (December 24, 2021): 1265–84. http://dx.doi.org/10.1093/mnras/stab3746.

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ABSTRACT Relativistic binary pulsars orbiting white dwarfs and neutron stars have already provided excellent tests of gravity. However, despite observational efforts, a pulsar orbiting a black hole has remained elusive. One possible explanation is the extreme Doppler smearing caused by the pulsar’s orbital motion which changes its apparent spin frequency during an observation. The classical solution to this problem has been to assume a constant acceleration/jerk for the entire observation. However, this assumption breaks down when the observation samples a large fraction of the orbit. This limits the length of search observations, and hence their sensitivity. This provides a strong motivation to develop techniques that can find compact binaries in longer observations. Here, we present a GPU-based radio pulsar search pipeline that can perform a coherent search for binary pulsars by directly searching over three or five Keplerian parameters using the template-bank algorithm. We compare the sensitivity obtained from our pipeline with acceleration and jerk search pipelines for simulated pulsar-stellar-mass black hole binaries and observations of PSR J0737−3039A. We also discuss the computational feasibility of our pipeline for untargeted pulsar surveys and targeted searches. Our benchmarks indicate that circular orbit searches for P-BH binaries with spin-period $P{_\mathrm{{spin}}} \ge {20}\, \mathrm{m\, s}$ covering the 3–10 Tobs regime are feasible for the High Time Resolution Universe pulsar survey. Additionally, an elliptical orbit search in Globular clusters for $P{_\mathrm{{spin}}} \ge {20}\, \mathrm{m\, s}$ pulsars orbiting intermediate-mass black holes in the 5–10 Tobs regime is feasible for observations shorter than 2 h with an eccentricity limit of 0.1.
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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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Taylor, J. H. "Binary Pulsars: Observations and Implications." Symposium - International Astronomical Union 125 (1987): 383–92. http://dx.doi.org/10.1017/s0074180900161005.

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The Galaxy contains a large number of neutron stars in gravitation-ally bound binary systems. Among the most fruitful of these to study have been the binary radio pulsars, of which seven are now known. Unlike the “accretion-powered” neutron stars located in mass-exchanging X-ray binary systems, the “rotation-powered” binary radio pulsars are found in dynamically simple, clean systems in which both stellar components have already completed their nuclear evolution, thereby shedding their atmospheres and most of their mass. In such circumstances the orbital parameters of the system and the rotational parameters of the pulsar can be determined with high precision from analysis of pulse timing data. These measurements constrain the component masses and yield an estimate of the pulsar's magnetic dipole moment, which turns out to be an essential parameter in understanding the evolution of the systems. In this paper I review the known facts concerning binary pulsars, and then briefly discuss some implications for our understanding of the place of neutron stars in stellar evolution.
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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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Bondonneau, Louis, Jean-Mathias Grießmeier, Gilles Theureau, and Maciej Serylak. "Low frequency pulsar observations with the international LOFAR station FR606." Proceedings of the International Astronomical Union 13, S337 (September 2017): 313–14. http://dx.doi.org/10.1017/s1743921317009656.

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AbstractThe pulsar’s signal passes through the interstellar medium (ISM) which leads to both chromatic dispersive delays and multipath pulse broadening. These effects have a strong frequency dependence (f−2 and f−4 respectively). Pulse profiles of pulsars are also frequency-dependent leading to some degeneracy with the ISM imprint. Furthermore, many pulsars show a turnover of their spectrum around ~100 MHz. For all these reasons, the frequency band below 100 MHz contains a lot of information about both the pulsar emission and the ISM. Our study is based on a LOw Frequency ARray (LOFAR) monitoring campaign using the international station FR606. Firstly, we demonstrate the importance of a monitoring campaign. Secondly, we calculate median spectra and locate the turnover frequency for 3 pulsars (B0809+74, B1133+16, B1508+55).
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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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Shearer, Andrew, and Eoin O’ Connor. "Optical pulsars and polarimetry." Proceedings of the International Astronomical Union 13, S337 (September 2017): 191–94. http://dx.doi.org/10.1017/s174392131700998x.

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AbstractDespite the early optical detection of the Crab pulsar in 1969, optical pulsars have become the poor cousin of the neutron star family. Only five normal pulsars have been observed to pulse in the optical waveband. A further three magnetars/SGRs have been detected in the optical/near IR. Optical pulsars are intrinsically faint with a first order luminosity, predicted by Pacini, to be proportional to P−10, where P is the pulsar’s period. Consequently they require both large telescopes, generally over-subscribed, and long exposure times, generally difficult to get. However optical observations have the benefit that polarisation and spectral observations are possible compared to X-ray and gamma-ray observations where polarisation measurements are limited. Over the next decade the number of optical pulsars should increase as optical detectors approach 100% quantum efficiency and as we move into the era of extremely large telescopes where limiting fluxes will be 30 to 100 times fainter compared to existing optical telescopes.
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Zhang, Xinyuan, Ping Shuai, Liangwei Huang, Shaolong Chen, and Lihong Xu. "Mission Overview and Initial Observation Results of the X-Ray Pulsar Navigation-I Satellite." International Journal of Aerospace Engineering 2017 (2017): 1–7. http://dx.doi.org/10.1155/2017/8561830.

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

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Kasian, Laura Elizabeth. "Radio observations of two binary pulsars." Thesis, University of British Columbia, 2012. http://hdl.handle.net/2429/41515.

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The study of pulsars in binary systems produces a wide variety of scientific results, including unique tests of general relativity and constraints on the equation of state of matter at extremely high densities. Through pulsar timing (which utilizes the fact that pulsars are precise clocks), it is possible to precisely measure the orbital parameters and masses of some binary pulsars, which can place constraints on their mass transfer histories. We present timing results for two binary pulsars. The intermediate-mass binary pulsar (IMBP) PSR J0621+1002 is a mildly recycled pulsar in an 8.3-day orbit around a massive white dwarf (WD) companion. It is one of only two known IMBPs with a precise mass measurement. We collected 9 days' worth of data using the 305-metre Arecibo telescope (allowing for full orbital coverage), which we used to improve constraints on the advance of periastron, and in turn, the pulsar and companion masses (to 1.53^{+0.10}_{-0.20}M☉ and 0.76^{+0.28}_{-0.07} solar masses, respectively) and inclination angle of the system. These results, combined with the relatively long orbital period, suggest a disk accretion evolutionary scenario involving short-lived periods of hyper-accretion, in which a moderate amount of mass has been transferred to the neutron star (NS). PSR J1906+0746 is a young pulsar in a compact ~4-hour orbit around a companion that was discovered in the early stages of the PALFA survey using the 305-metre Arecibo telescope. We present the timing results using data collected between 2005 to 2009 using the Green Bank, Arecibo, and Nançay telescopes. We have measured the advance of periastron, the time dilation and gravitational redshift parameter, and the orbital decay, and we find the pulsar and companion masses to be 1.323^{+0.011}_{-0.011}M☉ and 1.290^{+0.011}_{-0.011} solar masses, respectively. Although the companion may be a second NS, it is more likely to be a massive WD. The system's evolution probably involved a substantial transfer of mass from the WD progenitor onto the NS progenitor through Roche-lobe overflow accretion, followed by the formation of the WD, and a short common envelope phase, and finally the ejection of the envelope and the pulsar-forming supernova.
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Inam, Sitki Cagdas. "X-ray Observations Of Accretion Powered Pulsars." Phd thesis, METU, 2004. http://etd.lib.metu.edu.tr/upload/12605552/index.pdf.

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In this thesis, X-ray observations of four accretion powered pulsars are presented. Using RXTE observations of 4U 1907+09, we found three new pulse periods of the source. We found that the source spun-down almost at a constant rate of $dot nu$ = (-3.54 $pm 0.02) times 10^{-14}$ Hz s$^{-1}$ for more than 15 years. Using RXTE observations, X-ray flux related spectral and timing features in 2S 1417-62 were, in general, interpreted as a sign of a disc accretion with a similar geometry with a varying mass accretion rate, whereas spectral and timing features of the low X-ray flux regions were interpreted as a sign of possible temporary accretion geometry change prior to the next periastron. Using XMM-Newton and RXTE observations of SAX J2103.5+4545, we discovered quasi periodic oscillations around 0.044 Hz (22.7 sec) while the source was spinning-up with a rate of $(7.4pm0.9)times10^{-13}$Hz s$^{-1}$. In the X-ray spectrum, we also found a soft component consistent with a blackbody emission with ${rm{kT}}sim1.9$keV. Using RXTE observations, we also studied spectral evolution of Her X-1
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Hotan, Aidan Wade, and n/a. "High-precision observations of relativistic binary and millisecond pulsars." Swinburne University of Technology, 2006. http://adt.lib.swin.edu.au./public/adt-VSWT20060822.151026.

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The technique of pulsar timing reveals a wealth of new information when a precision of ∼1 μs or better is reached, but such precision is difficult to achieve. This thesis describes a series of very high precision timing observations that improve our knowledge of the targeted pulsar systems. We begin by describing a newly-developed baseband recording and coherent dedispersion system (CPSR2), along with a new object-oriented software development environment for pulsar data processing. Data obtained with this new instrument during a 3 year observing campaign at the Parkes 64m radio telescope are analysed in a number of novel ways. The mean profile of PSR J1022+1001 is shown to be stable on timescales of a few minutes, in contrast with previously published claims. We obtain a level of precision an order of magnitude better than any previous timing of this pulsar. In addition, we observe dramatic changes in the mean profile of the relativistic binary pulsar J1141?6545, which broadens by ∼50% over the time span of our observations. This is interpreted as evidence for secular evolution of the line of sight to the emission cone, caused by General relativistic geodetic precession which tilts the spin axis of the pulsar. High precision CPSR2 observations of the extraordinary double pulsar binary system are presented and we construct calibrated, mean polarimetric profiles for PSR J0737?3039A, in two frequency bands. These profiles provide a reference against which future profile evolution may be detected, given that we expect geodetic precession to alter the observed mean profile on an even shorter time scale than for PSR J1141?6545. The bulk of this thesis involves timing a selection of millisecond pulsars whose physical characteristics should allow the highest precision to be obtained. We measure several new proper motions and parallax distances. Shapiro delay is used to constrain the inclination angles and component masses of several of the binary systems in our source list. In addition, subtle periodic variations of the orbital parameters of two nearby binary millisecond pulsars are detected and attributed to annual orbital parallax, providing additional constraints on their three-dimensional orbital geometries. Future observations of these two sources may lead to more stringent tests of post-Keplerian gravitational theories. Finally, we use the timing residuals of one very stable source (PSR J1909?3744) as a reference against which we time PSR J1713+0747 with a root-mean-square precision of 133 ns, amongst the best timing residuals ever obtained. This result is an important step in the search for long-period gravitational waves using pulsar timing arrays.
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Hotan, Aidan Wade. "High-precision observations of relativistic binary and millisecond pulsars." Australasian Digital Theses Program, 2006. http://adt.lib.swin.edu.au/public/adt-VSWT20060822.151026.

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Thesis (PhD) - Swinburne University of Technology, 2006.
A dissertation presented in fulfillment of the requirements for the degree of Doctor of Philosophy, Swinburne University of Technology - 2006. Typescript. Includes bibliographical references (p. 182-190).
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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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Flanagan, Claire Susan. "Observations of glitches in PSR 0833-45 and 1641-45." Thesis, Rhodes University, 1996. http://hdl.handle.net/10962/d1005266.

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An eleven-year series of radio timing observations of 0833- 45 (Vela) and PSR 1641- 45 is presented. During this time, five large spin-ups ("glitches") were observed in 0833- 45 and one in 1641-45. The stellar response to these events is investigated, and the three relat ively long complete inter-glitch intervals in 0833-45 are modeled. The results are of relevance to studies of the interiors of neutron stars. The initial aim of the project - to obtain good observational coverage of large glitches in the Vela pulsar - was successfully achieved, and high quality observations of the periods between glitches were obtained as a by-product. The results of the analysis presented here provide support for the existence of both linear and non-linear coupling in the Vela pulsar, and put a limit on the former in PSR 1641- 45. The recently observed existence of a rapidly recovering component of part of a glitch in Vela was verified in the subsequent glitch, although there is now evidence to contradict the suggestion that this component involves a particular region of the star that is implicated in every glitch. Observations of a recent glitch in the same pulsar have resolved a small component of the spin-up; such a component has not been reported for any other large glitch.
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Parent, Damien. "Observations de pulsars avec le Fermi Gamma-ray Space Telescope." Phd thesis, Université Sciences et Technologies - Bordeaux I, 2009. http://tel.archives-ouvertes.fr/tel-00461405.

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Le Large Area Telescope à bord du satellite Fermi, lancé le 11 juin 2008, est un télescope spatial observant l'univers des hautes énergies. L'instrument couvre l'intervalle en énergie de 20MeV à 300 GeV avec une sensibilité nettement améliorée et la capacité de localiser des sources ponctuelles. Il détecte les photons gamma par leur conversion en paire électron-positron, et mesure leur direction et leur énergie grâce à un trajectographe et un calorimètre. Cette thèse présente les courbes de lumières et les mesures spectrales résolues en phase des pulsars radio et gamma détectés par le LAT. La mesure des paramètres spectraux (flux, indice spectral, et énergie de coupure) dépend des fonctions de réponse de l'instrument (IRFs). Une méthode développée pour la validation en orbite de la surface ecace est présentée en utilisant le pulsar de Vela. Les efficacités des coupures entre les données du LAT et les données simulées sont comparées à chaque niveau de la rejection du fond. Les résultats de cette analyse sont propagés vers les IRFs pour évaluer les systématiques des mesures spectrales. La dernière partie de cette thèse présente les découvertes de nouveaux pulsars individuels tels que PSR J0205+6449, J2229+6114, et J1048-5832 à partir des données du LAT et des éphémérides radio et X. Des analyses temporelles et spectrales sont investies dans le but de contraindre les modèles d'émission gamma. Finalement, nous discutons les propriétés d'une large population de pulsars gamma détectés par le LAT, incluant les pulsars normaux et les pulsars milliseconde.
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Huang, Hsiu-Hui. "X-ray and Optical observations of Globular Clusters and Pulsars." Diss., lmu, 2010. http://nbn-resolving.de/urn:nbn:de:bvb:19-123830.

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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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Kern, Brian. "Optical pulse-phased observations of faint pulsars with a phase-binning CCD camera." Diss., Pasadena, Calif. : California Institute of Technology, 2002. http://resolver.caltech.edu/CaltechETD:etd-06042002-125011.

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Books on the topic "Pulsars – Observations"

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

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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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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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A, Remillard Ronald, Woo Jonathan W, and United States. National Aeronautics and Space Administration., eds. ROSAT observations of a new X-ray transient in the small Magellanic cloud. [Washington, DC: National Aeronautics and Space Administration, 1997.

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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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United States. National Aeronautics and Space Administration., ed. Multiwavelength observations of unidentified high energy gamma-ray sources: Annual status report for NAG 5-2051. [Washington, D.C.]: National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. Multiwavelength observations of unidentified high energy gamma-ray sources: Annual status report for NAG 5-2051. [Washington, D.C.]: National Aeronautics and Space Administration, 1995.

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United States. National Aeronautics and Space Administration., ed. Multiwavelength observations of unidentified high energy gamma-ray sources: Combined annual status report & final technical report for NAG 5-2051. [Washington, DC: National Aeronautics and Space Administration, 1993.

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United States. National Aeronautics and Space Administration., ed. Multiwavelength observations of unidentified high energy gamma-ray sources: Combined annual status report & final technical report for NAG 5-2051. [Washington, DC: National Aeronautics and Space Administration, 1993.

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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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Book chapters on the topic "Pulsars – Observations"

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Lyne, A. G. "Observations of Pulsars." In High Energy Phenomena Around Collapsed Stars, 121–43. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3823-6_6.

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Laurent, P. "Sigma Observations of Pulsars." In The Lives of the Neutron Stars, 405–8. Dordrecht: Springer Netherlands, 1995. http://dx.doi.org/10.1007/978-94-011-0159-2_41.

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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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Taylor, J. H. "Binary Pulsars: Observations and Implications." In The Origin and Evolution of Neutron Stars, 383–92. Dordrecht: Springer Netherlands, 1987. http://dx.doi.org/10.1007/978-94-009-3913-4_72.

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Fruchter, A. S., and W. M. Goss. "Continuum Observations of Recycled Pulsars." In X-Ray Binaries and Recycled Pulsars, 105–13. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_12.

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Taylor, J. H. "Recent Observations of Recycled Pulsars." In X-Ray Binaries and Recycled Pulsars, 87–92. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_9.

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Wang, Na, R. N. Manchester, Aili Yusup, Xinji Wu, Jin Zhang, and Maozheng Chen. "Scintillation Observations Of Strong Northern Pulsars." In Sources and Scintillations, 57–60. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-1001-6_10.

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Shuai, Ping. "Observations of Radio and X-ray Pulsars." In Navigation: Science and Technology, 41–85. Singapore: Springer Singapore, 2021. http://dx.doi.org/10.1007/978-981-16-1067-7_2.

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Pilia, M., and A. Pellizzoni. "AGILE observations of PSR B1509-58." In High-Energy Emission from Pulsars and their Systems, 219–24. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-17251-9_18.

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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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Conference papers on the topic "Pulsars – Observations"

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

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Kildea, J., C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "VERITAS Observations of Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900312.

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

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Mignani, R. P., S. Zaggia, D. Dobrzycka, G. Beccari, A. de Luca, S. Mereghetti, P. A. Caraveo, et al. "VLT observations of Compact Central Objects." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900175.

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Yakovlev, D. G., O. Y. Gnedin, A. D. Kaminker, A. Y. Potekhin, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Theory of cooling neutron stars versus observations." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900259.

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Słowikowska, Agnieszka, Bronisław Rudak, Gottfried Kanbach, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "High energy polarization of pulsars—observations vs. models." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900128.

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Corongiu, A., A. Possenti, N. D'Amico, M. Burgay, A. G. Lyne, R. N. Manchester, F. Camilo, et al. "Parkes Observations of Radio Pulsars in Globular Clusters." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900306.

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Stappers, B. W., R. Karappusamy, J. W. T. Hessels, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Low Frequency Observations of Millisecond Pulsars with the WSRT." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900304.

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Ho, Wynn C. G., Kaya Mori, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Modeling Phase-resolved Observations of the Surfaces of Magnetic Neutron Stars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900178.

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Prince, Thomas A., Lars Bildsten, Deepto Chakrabarty, Robert B. Wilson, and Mark H. Finger. "Observations of accreting pulsars." In The evolution of X-ray binaries. AIP, 1994. http://dx.doi.org/10.1063/1.46016.

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Reports on the topic "Pulsars – Observations"

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

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

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Wilkins, Justin, Alexandria Barkman, Alexi Meltel, Burton Suedel, and Robert Richmond. Effects of sedimentation on three Hawaiian coral species under laboratory conditions. Engineer Research and Development Center (U.S.), August 2023. http://dx.doi.org/10.21079/11681/47541.

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Abstract:
Sedimentation can occur near a dredge operation in pulses over days, and potentially impact coral reefs occurring in close proximity. To improve the ability to predict the effects of dredging on corals, the effects of sedimentation in two 18-day experiments were studied for three common coral species representing different morphologies. In a laboratory setting, coral fragments were exposed to four sedimentation concentrations dosed every four days ranging from 0 to 60 mg cm-2. Separate experiments were performed in series, once with fine grain sediment and repeated with a coarse grain sediment. A 30-day sediment free observation period followed each experiment. Coral responses were measured throughout the experiment and at the end of the 18-day exposure and 30-day sediment free observation period. Photosynthetic yield, lipid ratios, tissue color, tissue loss, growth, and sediment cover varied among the treatment groups. All coral species were minimally affected when sediment concentrations were at or below 6 mg cm-2. P. meandrina and P. lobata experienced the most sediment coverage and tissue loss when exposed to sediment concentrations >30 mg cm-2 for either sediment. M. capitata experienced no sediment coverage or tissue loss when exposed to either sediment, but a reduction in photosynthetic yield at 60 mg cm-2 fine grain sediment was observed. During the 30-day post-exposure sediment free observation period, P. meandrina tissue loss continued, P. lobata nearly completely regrew lost tissue, while M. capitata showed no lingering effects. This study improves the US Army Corps of Engineers (USACE) ability to estimate the impacts of dredging on coral reefs.
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