Готові списки джерел за темами / X-­ray pulsars

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Автор: Grafiati
Опубліковано: 6 вересня 2023

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Статті в журналах з теми "X-­ray pulsars"

1

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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2

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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3

Becker, W. "X-ray Emission Characteristics of Pulsars." Symposium - International Astronomical Union 195 (2000): 49–60. http://dx.doi.org/10.1017/s0074180900162771.

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Recent X-ray observatories such as ROSAT, ASCA, RXTE, BeppoSAX, and Chandra have achieved important progress in neutron star and pulsar astronomy. The identification of Geminga as a rotation-powered pulsar, the discovery of X-ray emission from millisecond pulsars, and the identification of cooling neutron stars are only a few of the fascinating results. In the following, I will give a brief review on the X-ray emission properties of rotation-powered pulsars and their wind nebulae.
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4

Wang, H. G., G. J. Qiao, and R. X. Xu. "Phase Offset of Rotation-Powered X-ray Pulsars." Symposium - International Astronomical Union 214 (2003): 224–26. http://dx.doi.org/10.1017/s0074180900194458.

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Combing the data of all the 10 rotation-powered pulsars that have measurements of relative phase of radio and X-ray pulses, we report here the behavior of radio/X-ray phase offset. We find that the radio/X-ray offset of normal pulsars does not show the trend of increase with increasing pulsar period as the radio/gamma-ray offset exhibits. The offset of millisecond pulsars is generally much less than that of the normal pulsars. Such phenomenon should also be taken into account by the high energy models for pulsars.
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5

Liang, Hao, Yafeng Zhan, and Chaowei Duan. "A Bayesian Classifier for X-Ray Pulsars Recognition." International Journal of Aerospace Engineering 2016 (2016): 1–10. http://dx.doi.org/10.1155/2016/1746925.

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Recognition for X-ray pulsars is important for the problem of spacecraft’s attitude determination by X-ray Pulsar Navigation (XPNAV). By using the nonhomogeneous Poisson model of the received photons and the minimum recognition error criterion, a classifier based on the Bayesian theorem is proposed. For X-ray pulsars recognition with unknown Doppler frequency and initial phase, the features of every X-ray pulsar are extracted and the unknown parameters are estimated using the Maximum Likelihood (ML) method. Besides that, a method to recognize unknown X-ray pulsars or X-ray disturbances is proposed. Simulation results certificate the validity of the proposed Bayesian classifier.
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6

Kawai, N., Keisuke Tamura, and S. Shibata. "New Detection of X-Ray Pulsar Nebulae by ASCA." Symposium - International Astronomical Union 188 (1998): 265–66. http://dx.doi.org/10.1017/s0074180900115062.

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X-ray images of rotation-powered pulsars were examined using ASCA Gas Imaging Spectrometer (GIS). The data sets are taken from those available in the ASCA public archive in the performance verification (PV) phase and the guest-observing (GO) phase 1. We detected diffuse X-ray sources in the vicinity of nine pulsars including five new detections. There are large variety in their morphology and spatial size. The high probability of finding such diffuse sources around pulsars suggests that they exist universally for all the active pulsars, and that they are powered by the pulsars. We propose that the pulsar-powered nebula is a good probe to measure the otherwise invisible energy flux dissipating from a pulsar into the surrounding space.
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7

Pivovaroff, M. J., V. M. Kaspi, and F. Camilo. "X-ray observations of the high magnetic field radio pulsar PSR J1814–1744." International Astronomical Union Colloquium 177 (2000): 349–50. http://dx.doi.org/10.1017/s0252921100059959.

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AbstractWe present X-ray observations of PSR J1814–1744, a 4 s radio pulsar with inferred surface dipole magnetic field strength 5.5 × 1013G recently discovered in the on-going Parkes multibeam survey. This pulsar’s spin parameters are very similar to those of anomalous X-ray pulsars (AXPs). X-ray emission is not detected from the position of the radio pulsar in observations withROSATandASCA. The derived upper flux limit implies an X-ray luminosity significantly smaller than those of all known AXPs. These results argue that magnetar mechanism invoked to explain X-ray emission from AXPs must depend on more than merely the inferred surface magnetic field strength as estimated fromPand.
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8

Aoki, Yu, Takahiro Enomoto, Yoichi Yatsu, Nobuyuki Kawai, Takeshi Nakamori, Jun Kataoka, and P. Saz Parkinson. "Searching for X-ray counterparts of Fermi Gamma-ray pulsars in Suzaku observations." Proceedings of the International Astronomical Union 7, S279 (April 2011): 317–18. http://dx.doi.org/10.1017/s1743921312013130.

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AbstractWe report the Suzaku follow-up observations of the Gamma-ray pulsars, 1FGL J0614,13328, J1044.55737, J1741.82101, and J1813.31246, which were discovered by the Fermi Gamma-ray observatory. Analysing Suzaku/XIS data, we detected X-ray counterparts of these pulsars in the Fermi error circle and interpreted their spectra with absorbed power-law functions. These results indicate that the origin of these X-ray sources is non-thermal emission from the pulsars or from Pulsar Wind Nebulae (PWNe) surrounding them. Moreover we found that J1741.82101 exhibits a peculiar profile: spin-down luminosity vs flux ratio between X- and gamma-rays is unusually large compared to usual radio pulsars.
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9

ANKAY, AŞKIN, SERKAN ŞAHIN, GÖKÇE KARANFIL, and EFE YAZGAN. "EARLY PHASES OF DIFFERENT TYPES OF ISOLATED NEUTRON STAR." International Journal of Modern Physics D 14, no. 06 (June 2005): 1075–82. http://dx.doi.org/10.1142/s0218271805006535.

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Two Galactic isolated strong X-ray pulsars seem to be in the densest environments compared to other types of Galactic pulsar. X-ray pulsar J1846-0258 can be in an early phase of anomalous X-ray pulsars and soft gamma repeaters if its average braking index is ~1.8–2.0. X-ray pulsar J1811-1925 must have a very large average braking index (~11) if this pulsar was formed by SN 386AD. This X-ray pulsar can be in an early phase of the evolution of the radio pulsars located in the region P ~ 50–150 ms and Ṗ ~ 10-14–10-16 ss -1 of the P–Ṗ diagram. X-ray/radio pulsar J0540-69 seems to be evolving in the direction to the dim isolated thermal neutron star region on the P–Ṗ diagram. Possible progenitors of different types of neutron star are also discussed.
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10

Pivovaroff, M. J., V. M. Kaspi, and E. V. Gotthelf. "ASCA observations of Galactic rotation-powered pulsars." International Astronomical Union Colloquium 177 (2000): 351–52. http://dx.doi.org/10.1017/s0252921100059960.

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AbstractWe have examined several archivalASCAobservations of Galactic radio pulsars, including PSRs B1046–58 and B1610–50. X-ray emission is detected from PSR B1046–58 with a significance of ∼5σ. We find no evidence for pulsations. We argue that the emission is from a spatially unresolved synchrotron nebula powered by the pulsar. The location of the X-ray counterpart within the 95% position error ellipse of the gamma-ray source 3EG J1048–5840 strengthens the claim of Kaspi et al. (2000) that PSR B1046–58 emitϒ-rays. X-ray emission from PSR B1610–50 is not detected. We use the X-ray luminosity upper limit to constrain the pulsar’s velocity ≲ 200km s−1, arguing against an association with the nearby supernova remnant Kes 32. Our results for these radio pulsars contradict previous reports of detections of large (tens of arc minutes) associated synchrotron nebulae.
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Дисертації з теми "X-­ray pulsars"

1

Gavriil, Fotis Panagiotis. "Magnetar-like x-ray bursts from anomalous x-ray pulsars." Thesis, McGill University, 2006. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=100371.

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The leading model for understanding the energetics of anomalous X-ray pulsars (AXPs) is that they are "magnetars"---young, isolated neutron stars powered by the decay of their enormous magnetic fields. The identification of AXPs as magnetars is motivated by the similarity of AXPs to another enigmatic class of sources, the Soft Gamma Repeaters (SGRs). We report on long-term monitoring of AXPs using the Rossi X-ray Timing Explorer (RXTE). We monitor AXPs with RXTE to study their rotational stability, to search for variations in their pulsed flux and pulsed morphology. During our regular monitoring observations we discovered multiple bursts from two AXPs: this was the first time such behavior has been observed from these sources. Prior to our monitoring campaign, the detection of bursts solely from SGRs was the principle difference between AXPs and SGRs. The first detection of AXP bursts came in Fall 2001 when we discovered two SCR-like X-ray bursts from the direction of AXP 1E 1048.1--5937. Due to RXTE's large (1° x 1°) field-of-view we could not unambiguously identify the AXP as the burster. Recently, we detected a third burst from the direction of this source as well as a simultaneous increase in the pulsar's pulsed emission---this clearly identified the AXP as the burster. The most outstanding demonstration of AXP bursting behavior came on 2002 June 18 when AXP 1E 2259+586 underwent a major outburst involving 80 bursts and several changes in the persistent and pulsed emission, including a huge pulsed flux enhancement, a pulse morphology change and a rotational glitch. We also find variations in the persistent emission of AXPs in the absence of an obvious outburst. For example, we discovered two pulsed flux flares from AXP 1E 1048.1--5937. Both flares lasted several months and had well resolved few-week-long rises. The long rise tunes of the flares is a phenomenon not previously reported for this class of object, but has a clear explanation within the context of the magnetar model. All these results imply a close relationship between AXPs and SGRs, which we now believe are both magnetars, and have posed significant challenges to competing models.
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2

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

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3

Tang, Pui-shan Anisia. "Thermal X-ray pulses resulting from pulsar glitches /." Hong Kong : University of Hong Kong, 1999. http://sunzi.lib.hku.hk/hkuto/record.jsp?B2089675X.

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4

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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5

吳國偉 and Kwok-wai Eddie Ng. "Neutrino production from accreting X-ray pulsars." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1993. http://hub.hku.hk/bib/B31211811.

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6

Ng, Kwok-wai Eddie. "Neutrino production from accreting X-ray pulsars /." [Hong Kong : University of Hong Kong], 1993. http://sunzi.lib.hku.hk/hkuto/record.jsp?B13745013.

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7

Icdem, Burcin. "Viscous Time Scale In Accreting Powered Pulsars And Anomalous X-ray Pulsars." Master's thesis, METU, 2011. http://etd.lib.metu.edu.tr/upload/12613373/index.pdf.

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In this thesis we analyse X-ray data of accretion powered low mass and high mass X-ray binaries to understand the nature of their accretion mechanisms by searching for some clues of viscous time-scales of their accretion discs, if they have, in their low frequency power density spectra created from their long-term X-ray observations, or by doing pulse timing analysis with much shorter X-ray data to detect the effects of torque fluctuations caused by the accreting material on the pulsar. The low mass and high mass X-ray binaries we analysed have breaks in their power density spectra, which are attributed to the role of viscosity in the formation of accretion discs. Although, the time-scales corresponding to these break frequencies are smaller than the predictions of the Standard theory of accretion discs, the sources give consistent results among themselves by displaying the expected correlation between their break and orbital frequencies. The correlation curve of LMXBs implies thicker appearing accretion discs than those assumed by the theory. The dichotomy of the HMXBs on this curve points out the different origins of accretion that these sources may have, and offers a way to distinguish the stellar-wind fed systems from the Roche-lobe overflow systems. The timing and spectral analysis of Swift J1626.6-5156 reveal a correlation between the spin-up rate and the luminosity of the source implying that the pulsar is accretion-powered. This correlation together with the characteristics of the X-ray spectra enables us to estimate the magnetic field and the distance of the source. The AXP 1E 2259+586 does not display any signs of viscous time-scale in its low frequency power density spectra, and its pulse timing analysis gives a much smaller torque noise value than that expected from accretion powered pulsars. In addition, the analysis results presented in this thesis reveal magnetar-like glitches which differ than those of radio pulsars, due to the presence of the strong magnetic field of the pulsar. These results eliminate the possibility that the AXP is an accretion-powered pulsar.
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8

Dib, Rim. "RXTE monitoring of 5 anomalous x-ray pulsars." Thesis, McGill University, 2009. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=66730.

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Anomalous X-ray Pulsars (AXPs) are a group of neutron stars that share several common properties. They are dubbed "anomalous'' because their observed luminosity exceeds the rate of loss of their rotational kinetic energy. According to the magnetar model, they are young, isolated neutron stars, powered by a large magnetic energy reservoir. Five of these AXPs (1E 2259+586, 4U 0142+61, RXS J170849.0-400910, 1E 1841-045, 1E 1048.1-5937) have been monitored with the Rossi X-ray Timing Explorer (RXTE) since 1997 (1998 for two of the sources). The goal of the monitoring program is to study the timing behaviour of these sources including glitches, and the radiative variability in the soft X-ray band including pulsed flux changes, pulse profile changes, and bursts. The program provides a detailed description of the evolving properties of these objects, which can then be used to test AXP models, such as the magnetar model. In this thesis, I present some of my co-authored contributions to the AXP monitoring program.

I first present a long-term (1998-2006) study of AXP 4U 0142+61 in which we show that from 2000 to 2006 the pulse profile of the pulsar slowly evolved, and the pulsed flux increased by 29+/-8%.

AXP 4U 0142+61 then entered an active phase in 2006 March that lasted several months and included several X-ray bursts. I present a study of the behaviour of AXP 4U 0142+61 during this active phase.

I then present a long-term (1998-2007) study of AXPs RXS J170849.0-400910 and 1E 1841-045 in which we report on four new glitches. We show that AXPs are very active glitchers and that some AXP glitch properties are challenging to interpret in standard glitch models. Furthermore, we note that AXP glitches appear to fall in two classes: radiatively loud and radiatively quiet.

Finally, I present a long-term (1997-2008) study of AXP 1E 1048.1-5937 in which we show that three timing events occurred cont
Les pulsars X anormaux (AXPs) sont des étoiles à neutrons qui partagent certaines propriétés spécifiques. Ils sont dits "anormaux'" car leur luminosité est supérieure au taux de perte de leur énergie de rotation. Selon le modèle des "magnétars'', ces pulsars sont des étoiles à neutrons jeunes, isolées, et dont la luminosité provient d'un grand réservoir d'énergie magnétique. Cinq de ces AXPs (1E 2259+586, 4U 0142+61, RXS J170849.0-400910, 1E 1841-045, 1E 1048.1-5937) sont sous observation depuis 1997 dans le cadre d'un programme de surveillance utilisant le Rossi X-ray Timing Explorer (RXTE). Le but de ce programme est d'étudier les propriétés temporelles de ces pulsars tels les changements soudains de fréquence, et d'étudier leurs propriétés radiatives tels les changements de flux pulsé, les changements de profil de pulse, et les sursauts d'énergie. Ce programme de surveillance aide à obtenir une description détaillée des propriétés de ces objets, qui servira à tester les modèles théoriques des AXPs, dont le modèle des "magnétars''. Dans cette thèse, je présente quelques-unes de mes contributions au programme de surveillance.

D'abord, je présente une étude à long terme (1998-2006) du AXP 4U 0142+61 où nous montrons qu'entre 2000 et 2006, le profil de pulse du pulsar a lentement évolué, et que le flux pulsé a augmenté de 29+/-8%.

Le AXP 4U 0142+61 est ensuite entré dans une phase active en mars 2006, dans laquelle il a émis plusieurs sursauts d'énergie. Je présente une étude du comportement du AXP 4U 0142+61 pendant cette phase active.

Ensuite, je présente une étude à long terme (1998-2007) des AXPs RXS J170849.0-400910 et 1E 1841-045. Dans cette étude, nous avons détecté quatre nouveaux changements soudains de fréquence. Nous montrons que dans le contexte de changements soudains de fréquence, les AXPs sont très actifs. Nous montrons auss
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9

Camero, Arranz Ascension. "Accreting X-Ray pulsars. The high energy picture." Doctoral thesis, Universitat de València, 2007. http://hdl.handle.net/10803/9484.

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El objetivo principal de esta tesis ha sido el estudio del comportamiento transitorio durante estallidos de distinto tipo, de una selección de pulsares acretores en rayos X, localizados en el plano galáctico.Con ello se pretende haber avanzado hacia una explicación más clara de la naturaleza de estas objetos binarios de alta masa (con estrella de neutrones como objeto compacto), así como de los mecanismos físicos que operan en este escenario. Para todo esto se han analizado datos de dos misiones espaciales:INTEGRA Y RXTE.El segundo objetivo ha sido el estudio de la zona del brazo galactico de Scutum. Al ser esta una región de fuerte absorción se cree de la existencia de sistemas del tipo anteriormente mencionado este todavía escondidos, y los cuales solo pueden ser descubiertos a altas energías. En esta tesis se han podido presentar resultados esperanzadores, con la detección de varios objetos posibles nuevos candidatos a pulsares acretores de rayos X.
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10

Gavriil, Fotis P. "Long-term monitoring of anomalous X-ray pulsars with the rossi x-ray timing explorer." Thesis, McGill University, 2001. http://digitool.Library.McGill.CA:80/R/?func=dbin-jump-full&object_id=33763.

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We report on the long-term monitoring of five anomalous X-ray Pulsars (AXPs) using the Rossi X-ray Timing Explorer (RXTE ). We present a phase-coherent timing ephemeris for 4U 0142+61, and show that it has rotated with high stability over 4.4 yr, with RMS phase deviation of 7% of the pulse period from a simple fit including only n and n&d2; . We show that 1E 1048.1-5937 shows significant deviations from simple spin-down such that phase-coherent timing has not been possible over time spans longer than a few months. We find that the deviations from simple spin down are not consistent with single "glitch" type events, nor are they consistent with radiative precession. We suggest that 1E 1048.1-5937 may be a transition object between the soft gamma-ray repeater and AXP populations, and the AXP most likely to one day undergo an outburst. We also report on the continued timing stability of 1E 2259.1+586, for which phase coherence has now been maintained over 4.5 yr, as well as on the detection of a significant n&d3; in RXS J170849.0-400910, consistent with recovery following a glitch. We note a possible correlation in which timing stability decreases with increasing n&d2; . We find no large variability in pulse morphology as a function of time. We present high signal-to-noise ratio average pulse profiles for each AXP, and consider them as a function of energy. We find a variety of different behaviors, and consider possible trends in the data. We also find no large variations in pulsed flux, and set la upper limits of ∼20--30% of the mean.
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Книги з теми "X-­ray pulsars"

1

NATO Advanced Research Workshop on "X-ray Binaries and the Formation of Binary and Millisecond Radio Pulsars" (1991 Santa Barbara, Calif.). X-ray binaries and recycled pulsars. Dordrecht: Kluwer Academic Publishers, 1992.

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2

Heuvel, E. P. J., and S. A. Rappaport, eds. X-Ray Binaries and Recycled Pulsars. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2.

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3

Lee, Speyer Jason, ed. Navigation in Space by X-ray Pulsars. New York: Springer Verlag, 2011.

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4

Emadzadeh, Amir Abbas, and Jason Lee Speyer. Navigation in Space by X-ray Pulsars. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-8017-5.

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5

Thorsett, Stephen Erik. [X-ray emission from two nearby millisecond pulsars: Final technical report]. Pasadena, CA: California Institute of Technology, 1994.

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6

Thorsett, Stephen Erik. [X-ray emission from two nearby millisecond pulsars: Final technical report]. Pasadena, CA: California Institute of Technology, 1994.

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7

Thorsett, Stephen Erik. [X-ray emission from two nearby millisecond pulsars: Final technical report]. Pasadena, CA: California Institute of Technology, 1994.

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8

M, Cordes James, Yadigaroglu I. -A, and United States. National Aeronautics and Space Administration., eds. X-ray emission from the Guitar Nebula. [Washington, DC: National Aeronautics and Space Administration, 1997.

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9

M, Cordes James, Yadigaroglu I. -A, and United States. National Aeronautics and Space Administration., eds. X-ray emission from the Guitar Nebula. [Washington, DC: National Aeronautics and Space Administration, 1997.

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10

United States. National Aeronautics and Space Administration, ed. [Analysis and interpretation of X-ray pulsars]: [final technical report]. [Washington, DC: National Aeronautics and Space Administration, 1987.

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Частини книг з теми "X-­ray pulsars"

1

Walter, Roland, and Carlo Ferrigno. "X-Ray Pulsars." In Handbook of Supernovae, 1–15. Cham: Springer International Publishing, 2016. http://dx.doi.org/10.1007/978-3-319-20794-0_74-1.

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2

Walter, Roland, and Carlo Ferrigno. "X-Ray Pulsars." In Handbook of Supernovae, 1385–99. Cham: Springer International Publishing, 2017. http://dx.doi.org/10.1007/978-3-319-21846-5_74.

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3

Feroci, Marco, and Paolo Soffitta. "X-ray Polarimeters." In High-Energy Emission from Pulsars and their Systems, 585–609. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-17251-9_48.

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4

Mereghetti, S. "The Anomalous X-Ray Pulsars." In The Neutron Star—Black Hole Connection, 351–68. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0548-7_27.

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5

Patruno, Alessandro, and Anna L. Watts. "Accreting Millisecond X-ray Pulsars." In Timing Neutron Stars: Pulsations, Oscillations and Explosions, 143–208. Berlin, Heidelberg: Springer Berlin Heidelberg, 2020. http://dx.doi.org/10.1007/978-3-662-62110-3_4.

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6

Kulkarni, S. R., J. Navarro, G. Vasisht, Y. Tanaka, and F. Nagase. "Millisecond Pulsars and Quiescent LMXBS." In X-Ray Binaries and Recycled Pulsars, 99–104. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_11.

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7

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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8

Lyne, A. G. "Millisecond Pulsars in Globular Clusters." In X-Ray Binaries and Recycled Pulsars, 79–86. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2704-2_8.

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9

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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10

Becker, Werner. "X-Ray Emission from Pulsars and Neutron Stars." In Neutron Stars and Pulsars, 91–140. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-540-76965-1_6.

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Тези доповідей конференцій з теми "X-­ray pulsars"

1

Dib, Rim, Victoria M. Kaspi, Fotis P. Gavriil, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Glitches in Anomalous X-ray Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900151.

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2

Israel, G. L., F. Bernardini, M. Burgay, N. Rea, A. Possenti, S. Dall'Osso, L. Stella, et al. "Transient Phenomena in Anomalous X-ray Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900152.

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3

Tam, Cindy R., Fotis P. Gavriil, Rim Dib, Victoria M. Kaspi, Peter M. Woods, Cees Bassa, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "The Variable X-ray and Near-IR Behavior of the Particularly Anomalous X-ray Pulsar 1E 1048.1–5937." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900160.

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4

Özel, Feryal, Tolga Güver, Ersin Göğüş, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "The Magnetic Fields of Anomalous X-ray Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900155.

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5

Rea, N., S. Zane, R. Turolla, M. Lyutikov, D. Götz, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "New results on magnetars' X-ray spectral modeling." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900167.

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6

Bogdanov, Slavko, Jonathan E. Grindlay, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "An X-ray View of Radio Millisecond Pulsars." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900321.

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7

Mereghetti, S. "The anomalous x-ray pulsars." In X-RAY ASTRONOMY: Stellar Endpoints,AGN, and the Diffuse X-ray Background. AIP, 2001. http://dx.doi.org/10.1063/1.1434635.

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Ray, Paul S., Michael T. Wolff, Paul Demorest, Ismaël Cognard, Donald C. Backer, Kent S. Wood, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "X-ray and Radio Timing of PSR B1821–24." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900134.

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9

Archibald, Anne M., Rim Dib, Margaret A. Livingstone, Victoria M. Kaspi, C. Bassa, Z. Wang, A. Cumming, and V. M. Kaspi. "Red Noise in Anomalous X-ray Pulsar Timing Residuals." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900158.

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10

Lommen, A., J. Donovan, C. Gwinn, Z. Arzoumanian, A. Harding, M. Strickman, R. Dodson, et al. "Observed X-ray∕Radio Correlation in the Vela Pulsar." In 40 YEARS OF PULSARS: Millisecond Pulsars, Magnetars and More. AIP, 2008. http://dx.doi.org/10.1063/1.2900322.

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Звіти організацій з теми "X-­ray pulsars"

1

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

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2

West, Gavin. Shaping X-Ray Pulses at LCLS - Oral Presentation. Office of Scientific and Technical Information (OSTI), August 2015. http://dx.doi.org/10.2172/1213173.

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3

Zholents, A. Electron beam-based sources of ultrashort x-ray pulses. Office of Scientific and Technical Information (OSTI), September 2010. http://dx.doi.org/10.2172/990520.

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4

Huang, Z. Femtosecond X-ray Pulses From a frequency chirped SASE FEL. Office of Scientific and Technical Information (OSTI), January 2003. http://dx.doi.org/10.2172/826693.

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5

Chin, A. H., R. W. Schoenlein, and T. E. Glover. Ultrashort hard x-ray pulses generated by 90 degrees Thomson scattering. Office of Scientific and Technical Information (OSTI), April 1997. http://dx.doi.org/10.2172/603713.

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6

Emma, P. ATTOSECOND X-RAY PULSES IN THE LCLS USING THE SLOTTED FOIL METHOD. Office of Scientific and Technical Information (OSTI), September 2004. http://dx.doi.org/10.2172/833050.

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7

Huang, Zhirong, and Ronald D. Ruth. Fully Coherent X-ray Pulses from a Regenerative Amplifier Free Electron Laser. Office of Scientific and Technical Information (OSTI), February 2006. http://dx.doi.org/10.2172/876447.

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Miao, J. Taking X-Ray Diffraction to the Limit: Macromolecular Structures from Femtosecond X-Ray Pulses and Diffraction Microscopy of Cells with Synchrotron Radiation. Office of Scientific and Technical Information (OSTI), June 2004. http://dx.doi.org/10.2172/826961.

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9

Emma, P. Femtosecond and Subfemtosecond X-Ray Pulses from a SASE Based Free-Electron Laser. Office of Scientific and Technical Information (OSTI), March 2004. http://dx.doi.org/10.2172/826765.

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10

Zholents, Alexander. Feasibility analysis for attosecond X-ray pulses at FERMI@ELETTRA free electron laser. Office of Scientific and Technical Information (OSTI), September 2004. http://dx.doi.org/10.2172/842992.

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