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Journal articles on the topic 'X-ray pulsars'

Author: Grafiati

Published: 6 September 2023

Last updated: 25 July 2025

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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 baryc

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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

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3

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 prop

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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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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 (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 th

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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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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 de

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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

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9

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

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10

Aoki, Yu, Takahiro Enomoto, Yoichi Yatsu, et al. "Searching for X-ray counterparts of Fermi Gamma-ray pulsars in Suzaku observations." Proceedings of the International Astronomical Union 7, S279 (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 luminos

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Xu 徐, Yu-Jing 雨婧, Han-Long 寒龙 Peng 彭, Shan-Shan 山杉 Weng 翁, Xiao 潇. Zhang 张, and Ming-Yu 明玉 Ge 葛. "A New X-Ray Census of Rotation Powered Pulsars." Astrophysical Journal 981, no. 2 (2025): 100. https://doi.org/10.3847/1538-4357/adaebc.

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Abstract To date, over 4000 pulsars have been detected. In this study, we identify 231 X-ray counterparts of Australia Telescope National Facility (ATNF) pulsars by performing a spatial cross match across the Chandra, XMM-Newton observational catalogs. This data set represents the largest sample of X-ray counterparts ever compiled, including 98 normal pulsars (NPs) and 133 millisecond pulsars (MSPs). Based on this significantly expanded sample, we re-establish the correlation between X-ray luminosity and spin-down power, given by L X ∝ E ̇ 0.85 ± 0.05 across the whole X-ray band. The strong co

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12

Becker, Werner. "X-ray emission characteristics of pulsars and their nebulae." International Astronomical Union Colloquium 177 (2000): 321–26. http://dx.doi.org/10.1017/s025292110005987x.

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AbstractRecent X-ray observatories like 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 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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13

Gotthelf, E. V., G. Vasisht, B. Gaensler, and K. Torii. "Discovery of a supernova remnant with a central X-ray source: AX J184453.3-025642 in G 29.6+0.1." International Astronomical Union Colloquium 177 (2000): 707–8. http://dx.doi.org/10.1017/s0252921100061030.

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AbstractWe report preliminary results from our follow-up X-ray and radio study of AX J1845–0258, the 7-s X-ray pulsar whose characteristics are similar to those found for the anomalous X-ray pulsars (AXPs). We have located a faint X-ray source within the pulsar’s error circle implying a dramatic reduction in flux, however, the source is too faint to provide a confirmation of the expected pulsations. Centered on this X-ray source is a newly discovered supernova remnant, evident in both radio and X-ray emission. This is the third example of an AXP-like object associated with a supernova remnant.

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Shearer, Andrew, and Eoin O’ Connor. "Optical pulsars and polarimetry." Proceedings of the International Astronomical Union 13, S337 (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 observa

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Brazier, K. T. S. "The X-ray synchrotron nebula around PSR 1509-58." International Astronomical Union Colloquium 160 (1996): 351–52. http://dx.doi.org/10.1017/s0252921100041853.

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PSR 1509-58 is one of the youngest and most powerful pulsars known and is visible not only in soft X-rays, but in gamma-rays. Observations of its supernova remnant (MSH 15-52) offer a rare chance to study such a young pulsar and to explore its surroundings, which in X-rays include the pulsar’s 10×6 arcmin X-ray synchrotron nebula and the peculiar, filamentary optical nebula, RCW 89, that sits on the limb of MSH 15-52 (Seward &amp; Harnden 1982, Seward et al. 1983). This paper will concentrate on the morphology of the synchrotron nebula.

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Dinsmore, Jack T., and Roger W. Romani. "A Catalog of Pulsar X-Ray Filaments." Astrophysical Journal 976, no. 1 (2024): 4. http://dx.doi.org/10.3847/1538-4357/ad8344.

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Abstract We present the first Chandra X-ray Observatory (CXO) catalog of “pulsar X-ray filaments,” or “misaligned outflows.” These are linear, synchrotron-radiating features powered by ultrarelativistic electrons and positrons that escape from bow shock pulsars. The filaments are misaligned with the (large) pulsar velocity, distinguishing them from the pulsar wind nebula (PWN) trail, which is also often visible in CXO ACIS images. Spectral fits and morphological properties are extracted for five secure filaments and three candidates using a uniform method. We present a search of archival CXO d

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Gotthelf, E. V., and G. Vasisht. "A New View on Young Pulsars in Supernova Remnants: Slow, Radio-quiet & X-ray Bright." International Astronomical Union Colloquium 177 (2000): 699–702. http://dx.doi.org/10.1017/s0252921100061017.

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AbstractWe propose a simple explanation for the apparent dearth of radio pulsars associated with young supernova remnants (SNRs). Recent X-ray observations of young remnants have revealed slowly rotating (P∼ 10s) central pulsars with pulsed emission above 2 keV, lacking in detectable radio emission. Some of these objects apparently have enormous magnetic fields, evolving in a manner distinct from the Crab pulsar. We argue that these X-ray pulsars can account for a substantial fraction of the long sought after neutron stars in SNRs and that Crab-like pulsars are perhaps the rarer, but more high

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Malov, I. F. "On the Mechanism of X-ray Emission from Radio Pulsars." Symposium - International Astronomical Union 218 (2004): 387–88. http://dx.doi.org/10.1017/s007418090018146x.

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The correlations between the luminosities of radio pulsars in various wavebands and the magnetic fields at the light cylinder suggest that the observed emission is generated in outer layers of the pulsar magnetospheres by the synchrotron mechanism. The formula for calculating the X-ray luminosity LX of radio pulsars is derived in the framework of the synchrotron model. It is shown that LX depends strongly on the parameter This raises the possibility of predicting the detection of X-ray emission from more than a hundred known radio pulsars.

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Jiang, Kun, Yusong Wang, Hui Yang, and Hong Yuan. "X-ray Pulsar-Based Navigation Using Pulse Phase Delay between Spacecraft and Verification with Real Data." Applied Sciences 14, no. 15 (2024): 6401. http://dx.doi.org/10.3390/app14156401.

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Pulsars are neutron stars with high rotation speeds and have extraordinary long-term rotational stability. X-ray pulsar-based navigation (XNAV) is a navigation method that estimates the position and velocity of a spacecraft using the X-ray radiation from pulsars. Flight experiments on Insight-Hard X-ray Modulation Telescope (Insight-HXMT) and Neutron Star Interior Composition Explorer (NICER) have successfully verified the feasibility of using XNAV for a single spacecraft. For spacecraft in formation, a pulsar-based navigation method that uses the pulse phase delay between spacecraft is derive

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Chen, Qiang, Yong Zhao, and Lixia Yan. "X-ray Pulsar Signal Denoising Based on Variational Mode Decomposition." Entropy 23, no. 9 (2021): 1181. http://dx.doi.org/10.3390/e23091181.

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Pulsars, especially X-ray pulsars detectable for small-size detectors, are highly accurate natural clocks suggesting potential applications such as interplanetary navigation control. Due to various complex cosmic background noise, the original pulsar signals, namely photon sequences, observed by detectors have low signal-to-noise ratios (SNRs) that obstruct the practical uses. This paper presents the pulsar denoising strategy developed based on the variational mode decomposition (VMD) approach. It is actually the initial work of our interplanetary navigation control research. The original puls

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Sullivan, Andrew G., and Roger W. Romani. "High-energy Emission from the Intrabinary Shocks in Redback Pulsars." Astrophysical Journal 984, no. 2 (2025): 146. https://doi.org/10.3847/1538-4357/adc720.

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Abstract The intrabinary shocks (IBS) of spider pulsars emit nonthermal synchrotron X-rays from accelerated electrons and positrons in the shocked pulsar wind, likely energized by magnetic reconnection. In redback spider pulsars, the IBS typically wraps around the pulsar, leading to a near-normal IBS shock with relatively bright X-ray emission. The characteristic energies of radiating particles and the magnetic fields in the IBS suggest spectral features in the hard X-ray band. Here, we perform joint soft–hard X-ray analyses of three redback pulsars, J1723-2837, J2215+5135, and J2339-0533, inc

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Gentile, P., M. McLaughlin, M. Roberts, et al. "Chandra observations of black widow pulsars." Proceedings of the International Astronomical Union 8, S291 (2012): 389–91. http://dx.doi.org/10.1017/s1743921312024234.

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AbstractWe describe the first X-ray observations of binary millisecond pulsars PSR J0023+0923, J1810+1744, J2215+5135, and J2256−1024. All are Fermi gamma-ray sources and three are ‘black-widow’ pulsars, with companions of mass < 0.1 M⊙. Data were taken using the Chandra X-Ray Observatory and covered a full binary orbit for each pulsar. PSRs J2215+5135 and J2256−1024, show significant orbital variability and X-ray flux minima coinciding with eclipses seen at radio wavelengths. This is consistent with intrabinary shock emission characteristic of black-widow pulsars. The other two pulsars, PS

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Gotthelf, E. V. "Correlation between the X-ray Spectra of Young Pulsars and their Wind Nebulae." Symposium - International Astronomical Union 214 (2003): 163–66. http://dx.doi.org/10.1017/s0074180900194331.

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A significant correlation is discovered between the X-ray spectra of young pulsars (PSRs) and that of their associated wind nebulae (PWNe). For a sample of nine bright Crab-like pulsar systems observed with the Chandra X-ray observatory, we report a linear relationship between the photon indices for the PWNe and those of the phase-averaged pulsar emission, where ΓPWN = 0.72 ± 0.13 × ΓPSR + 0.86 ± 0.20. Furthermore, we find that the spectral slopes of younger, more energetic, pulsars tend to be steeper. These results confirm a consistent pulsar emission mechanism and provide important new obser

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Klingler, Noel, Jeremy Hare, Oleg Kargaltsev, George G. Pavlov, and John Tomsick. "A NuSTAR and Chandra Investigation of the Misaligned Outflow of PSR J1101–6101 and the Lighthouse Pulsar Wind Nebula." Astrophysical Journal 950, no. 2 (2023): 177. http://dx.doi.org/10.3847/1538-4357/accd60.

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Abstract PSR J1101–6101 is an energetic young pulsar that powers the remarkable Lighthouse pulsar wind nebula (PWN). The pulsar belongs to the rare type of radio- and gamma-ray-quiet pulsars that are bright in hard X-rays. Moreover, the Lighthouse PWN is remarkable for its misaligned outflow (which gave rise to the PWN’s nickname). Also known as “pulsar filaments,” these collimated parsec-scale X-ray structures have been recently discovered in the vicinity of a handful of fast-moving pulsars, and they appear unaffected by the ram pressure that confines pulsar tails. We report on NuSTAR observa

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Yang, Bo, and Ling Ke Liu. "Deep Space Navigation Using X-Ray Pulsars." Advanced Materials Research 433-440 (January 2012): 6325–31. http://dx.doi.org/10.4028/www.scientific.net/amr.433-440.6325.

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This paper presents a novel technology for determining spacecraft position and velocity using X-ray pulsars. There are numerous potential benefits from this technology. A X-ray pulsar-based navigation (XNAV) system would be available anywhere in the Solar System that cosmic X-ray sources can be observed. The relatively low disturbance environment of deep space, as compared with low-Earth orbit, allows pulse time of arrival (TOA) to be measured precisely. Furthermore, the system require only infrequent pulsar ephemeris updates and can operate in an autonomous mode, independent of Deep Space Net

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Paduano, Alessandro, Arash Bahramian, James C. A. Miller-Jones, et al. "The MAVERIC Survey: Simultaneous Chandra and VLA observations of the transitional millisecond pulsar candidate NGC 6652B." Monthly Notices of the Royal Astronomical Society 506, no. 3 (2021): 4107–20. http://dx.doi.org/10.1093/mnras/stab1928.

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ABSTRACT Transitional millisecond pulsars are millisecond pulsars that switch between a rotation-powered millisecond pulsar state and an accretion-powered X-ray binary state, and are thought to be an evolutionary stage between neutron star low-mass X-ray binaries and millisecond pulsars. So far, only three confirmed systems have been identified in addition to a handful of candidates. We present the results of a multiwavelength study of the low-mass X-ray binary NGC 6652B in the globular cluster NGC 6652, including simultaneous radio and X-ray observations taken by the Karl G. Jansky Very Large

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Ulmer, M. P. "Gamma-Ray Observations of Pulsars." International Astronomical Union Colloquium 142 (1994): 789–95. http://dx.doi.org/10.1017/s0252921100078106.

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AbstractWe report on Compton Gamma Ray Observatory observations of six detected pulsars: the Crab, Vela, Geminga, PSR B1509-58, PSR B1706-44, and PSR B1055-52. We combine these data with radio data and X-ray data to provide an overview of what is known about gamma-ray pulsars. We discuss light curves, spectra, and radio/gamma-ray phase offsets, and present several tentative patterns in the data. These include constant phase with γ-ray energy; a correlation between gamma-ray and X-ray luminosity; an anticorrelation between the gamma-ray luminosity and the efficiency in converting rotational ene

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GUSEINOV, OKTAY H., AŞKIN ANKAY, SEVINÇ O. TAGIEVA, and M. ÖZGÜR TAŞKIN. "DEPENDENCE OF THE X-RAY LUMINOSITY AND PULSAR WIND NEBULA ON DIFFERENT PARAMETERS OF PULSARS AND THE EVOLUTIONARY EFFECTS." International Journal of Modern Physics D 13, no. 02 (2004): 197–213. http://dx.doi.org/10.1142/s0218271804004505.

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Dependences of the X-ray luminosity (Lx) of young single pulsars, due to ejection of relativistic particles, on electric field intensity, rate of rotational energy loss (Ė), magnetic field, period, and some other parameters of neutron stars are discussed. Influence of the magnetic field and effects of some other parameters of neutron stars on the Lx-Ė and the Lx-τ (characteristic time) dependences are considered. Evolutionary factors also play an important role in our considerations. Only the pulsars with L2–10 keV >1033 erg/s have pulsar wind nebula around them. The pulsars from which γ-ra

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Vahdat, A., B. Posselt, A. Santangelo, and G. G. Pavlov. "Toward an X-ray inventory of nearby neutron stars." Astronomy & Astrophysics 658 (February 2022): A95. http://dx.doi.org/10.1051/0004-6361/202141795.

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Context. The X-ray emission of neutron stars enables a probe of their temperatures, geometries and magnetospheric properties. The current number of X-ray emitting pulsars is insufficient to rule out observational biases that may arise from poorly known distance, age, or location of the neutron stars. One approach to overcome such biases is to create a distance-limited sample with sufficiently deep observations. Aims. With the aim of better sampling of the nearby (≲2 kpc) population of neutron stars, we started an XMM-Newton survey of pulsars to measure their X-ray fluxes or derive respective c

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Nagase, F. "Results of the Timing Analyses of X-ray Pulsars Observed by Hakucho and Tenma." Symposium - International Astronomical Union 125 (1987): 200. http://dx.doi.org/10.1017/s0074180900160735.

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A dozen of X-ray pulsars have been observed with the Japanese X-ray astronomy satellites Hakucho and Tenma between 1979 and 1984. The obsetvations revealed remarkable pulse period changes both in disk-fed and wind-fed pulsars. From the histories of the pulse period changes so far measured, we are able to classify the X-ray pulsars into three categories: (1)Pulsars which exhibit a steady spin-up with a constant rate of period change (e.g., 4U 1626-67 and GX 1+4).(2)Disk-fed pulsars in which considerable period changes are superposed on the secular trend of spin-up (e.g., Her X-1 and Cen X-3).(3

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Lobato, Ronaldo V., Manuel Malheiro, and Jaziel G. Coelho. "Magnetars and white dwarf pulsars." International Journal of Modern Physics D 25, no. 09 (2016): 1641025. http://dx.doi.org/10.1142/s021827181641025x.

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The anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are a class of pulsars understood as neutron stars (NSs) with super strong surface magnetic fields, namely [Formula: see text][Formula: see text]G, and for that reason are known as magnetars. However, in the last years, some SGRs/AXPs with low surface magnetic fields [Formula: see text]–[Formula: see text][Formula: see text]G have been detected, challenging the magnetar description. Moreover, some fast and very magnetic white dwarfs (WDs) have also been observed, and at least one showed X-ray energy emission as an ordinary

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Tauris, T. M. "On the connection between accreting X-ray and radio millisecond pulsars." Proceedings of the International Astronomical Union 8, S290 (2012): 141–44. http://dx.doi.org/10.1017/s1743921312019394.

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AbstractFor many years it has been recognized that the terminal stages of mass transfer in a low-mass X-ray binary (LMXB) should cause the magnetosphere of the accreting neutron star to expand, leading to a braking torque acting on the spinning pulsar. After the discovery of radio millisecond pulsars (MSPs) it was therefore somewhat a paradox (e.g. Ruderman et al. 1989) how these pulsars could retain their fast spins following the Roche-lobe decoupling phase, RLDP. Here I present a solution to this so-called “turn-off problem” which was recently found by combining binary stellar evolution mode

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COELHO, J. G., and M. MALHEIRO. "SIMILARITIES OF SGRs WITH LOW MAGNETIC FIELD AND WHITE DWARF PULSARS." International Journal of Modern Physics: Conference Series 18 (January 2012): 96–100. http://dx.doi.org/10.1142/s2010194512008276.

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Some of the most interesting types of astrophysical objects that have been intensively studied in the recent years are the Anomalous X-ray Pulsars (AXPs) and Soft Gamma-ray Repeaters (SGRs) seen usually as neutron stars pulsars with super strong magnetic fields. However, in the last two years two SGRs with low magnetic fields have been detected. Moreover, fast and very magnetic white dwarf pulsars have also been observed in the last years. Based on these new pulsar discoveries, white dwarf pulsars have been proposed as an alternative explanation to the observational features of SGRs and AXPs.

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Bogdanov, Slavko. "X-rays from Radio Millisecond Pulsars." Proceedings of the International Astronomical Union 13, S337 (2017): 116–19. http://dx.doi.org/10.1017/s1743921317011553.

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AbstractThe Galactic population of rotation-powered (aka radio) millisecond pulsars (MSPs) exhibits diverse X-ray properties. Energetic MSPs show pulsed non-thermal radiation from their magnetospheres. Eclipsing binary MSPs predominantly have X-ray emission from a pulsar wind driven intra-binary shock. Typical radio MSPs emit X-rays from their heated magnetic polar caps. These thermally emitting MSPs offer the opportunity to place interesting constraints on the long sought after dense matter equation of state, making them important targets of investigation of the recently deployed Neutron Star

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35

McLaughlin, M. A., D. R. Lorimer, A. G. Lyne, et al. "Two Radio Pulsars with Magnetar Fields." Symposium - International Astronomical Union 218 (2004): 255–56. http://dx.doi.org/10.1017/s0074180900181094.

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PSRs J1847–0130 and J1718–37184 have inferred surface dipole magnetic fields greater than those of any other known pulsars and well above the “quantum critical field” above which some models predict radio emission should not occur. These fields are similar to those of the anomalous X-ray pulsars (AXPs), which growing evidence suggests are “magnetars”. The lack of AXP-like X-ray emission from these radio pulsars (and the non-detection of radio emission from the AXPs) creates new challenges for understanding pulsar emission physics and the relationship between these classes of apparently young n

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36

Strader, Jay, Paul S. Ray, Ryan Urquhart, et al. "PSR J1947−1120: A New Huntsman Millisecond Pulsar Binary." Astrophysical Journal 980, no. 1 (2025): 124. https://doi.org/10.3847/1538-4357/ada897.

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Abstract We present the discovery of PSR J1947–1120, a new huntsman millisecond pulsar with a red giant companion star in a 10.3 day orbit. This pulsar was found via optical, X-ray, and radio follow-up of the previously unassociated γ-ray source 4FGL J1947.6–1121. PSR J1947–1120 is the second confirmed pulsar in the huntsman class and establishes this as a bona fide subclass of millisecond pulsars. We use MESA models to show that huntsman pulsars can be naturally explained as neutron star binaries whose secondaries are currently in the “red bump” region of the red giant branch, temporarily und

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Dodson, Richard, Dion Lewis, David Legge, et al. "The Vela Pulsar, the Key?" Symposium - International Astronomical Union 218 (2004): 193–94. http://dx.doi.org/10.1017/s0074180900180945.

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Of all pulsars known, Vela has been one of the most productive in terms in understanding pulsars and their characteristics. We present the latest results derived from Australian telescopes. These include a more accurate pulsar distance, a more precise pulsar local space velocity, a new model of spin-up at a glitch, and the association of a radio nebula with the X-ray pulsar wind nebula.

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Poutanen, Juri, Sergey S. Tsygankov, and Sofia V. Forsblom. "X-ray Polarimetry of X-ray Pulsars." Galaxies 12, no. 4 (2024): 46. http://dx.doi.org/10.3390/galaxies12040046.

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Radiation from X-ray pulsars (XRPs) was expected to be strongly linearly polarized owing to a large difference in their ordinary and extraordinary mode opacities. The launch of IXPE allowed us to check this prediction. IXPE observed a dozen X-ray pulsars, discovering pulse-phase dependent variation of the polarization degree (PD) and polarization angle (PA). Although the PD showed rather erratic profiles resembling flux pulse dependence, the PA in most cases showed smooth variations consistent with the rotating vector model (RVM), which can be interpreted as a combined effect of vacuum birefri

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Forsblom, Sofia V., Juri Poutanen, Sergey S. Tsygankov, et al. "IXPE Observations of the Quintessential Wind-accreting X-Ray Pulsar Vela X-1." Astrophysical Journal Letters 947, no. 2 (2023): L20. http://dx.doi.org/10.3847/2041-8213/acc391.

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Abstract The radiation from accreting X-ray pulsars was expected to be highly polarized, with some estimates for the polarization degree of up to 80%. However, phase-resolved and energy-resolved polarimetry of X-ray pulsars is required in order to test different models and to shed light on the emission processes and the geometry of the emission region. Here we present the first results of the observations of the accreting X-ray pulsar Vela X-1 performed with the Imaging X-ray Polarimetry Explorer. Vela X-1 is considered to be the archetypal example of a wind-accreting, high-mass X-ray binary s

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40

Poutanen, Juri. "Relativistic rotating vector model for X-ray millisecond pulsars." Astronomy & Astrophysics 641 (September 2020): A166. http://dx.doi.org/10.1051/0004-6361/202038689.

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The X-ray radiation produced on the surface of accreting magnetised neutron stars is expected to be strongly polarised. A swing of the polarisation vector with the pulsar phase gives a direct measure of the source inclination and magnetic obliquity. In the case of rapidly rotating millisecond pulsars, the relativistic motion of the emission region causes additional rotation of the polarisation plane. Here, we develop a relativistic rotating vector model, where we derive analytical expression for the polarisation angle as a function of the pulsar phase accounting for relativistic aberration and

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Gallant, Y. A., R. Bandiera, N. Bucciantini, and E. Amato. "Constraining pulsar birth properties with supernova X-ray observations." Proceedings of the International Astronomical Union 12, S331 (2017): 63–68. http://dx.doi.org/10.1017/s1743921317004756.

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AbstractA large fraction of core-collapse supernovae are thought to result in the birth of a rotation-powered pulsar, which is later observable as a radio pulsar up to great ages. The birth properties of these pulsars, and in particular the distribution of their initial rotation periods, are however difficult to infer from studies of the radio pulsar population in our Galaxy. Yet the distributions of their birth properties is an important assumption for scenarios in which ultra-high-energy cosmic rays (UHECRs) originate in very young, extragalactic pulsars with short birth periods and/or high

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Kaspi, V. M., and F. P. Gavriil. "(Anomalous) X-ray Pulsars." Nuclear Physics B - Proceedings Supplements 132 (June 2004): 456–65. http://dx.doi.org/10.1016/j.nuclphysbps.2004.04.080.

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Gotthelf, E. V. "A Spin-down Power Threshold for Pulsar Wind Nebula Generation?" Symposium - International Astronomical Union 218 (2004): 225–28. http://dx.doi.org/10.1017/s0074180900181045.

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A systematic X-ray survey of the most energetic rotation-powered pulsars known, based on spin-down energy loss rate, shows that all energetic pulsars with Ė > Ėc ≍ 4 × 1036 ergs s−1 are X-ray-bright, manifest a distinct pulsar wind nebula (PWN), and are associated with a supernova event, with over half residing in shell-like supernova remnants. Below Ėc, the 2–10 keV flux ratio FPWN/FPSR decreases by an order-of-magnitude. This threshold is consistent with the lower limit on the spectral slope γmin ≍ 0.6 observed for rotation-powered pulsars (Gotthelf 2003). The apparent lack of bright PWNe

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Ay, Fahrettin, Gökhan İnce, Mustafa E. Kamaşak, and K. Yavuz Ekşi. "Classification of pulsars with Dirichlet process Gaussian mixture model." Monthly Notices of the Royal Astronomical Society 493, no. 1 (2020): 713–22. http://dx.doi.org/10.1093/mnras/staa154.

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ABSTRACT Young isolated neutron stars (INSs) most commonly manifest themselves as rotationally powered pulsars that involve conventional radio pulsars as well as gamma-ray pulsars and rotating radio transients. Some other young INS families manifest themselves as anomalous X-ray pulsars and soft gamma-ray repeaters that are commonly accepted as magnetars, i.e. magnetically powered neutron stars with decaying super-strong fields. Yet some other young INSs are identified as central compact objects and X-ray dim isolated neutron stars that are cooling objects powered by their thermal energy. Olde

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Liu, Li, Wei Zheng, and Guojian Tang. "Autonomous Positioning of Satellite Constellations via X-ray Pulsar Measurements." Journal of Navigation 66, no. 5 (2013): 671–82. http://dx.doi.org/10.1017/s0373463313000325.

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A novel autonomous positioning approach based on X-ray pulsars is proposed in this paper. First, the principles of the pulsar–based measurement model and the inter-satellite range model in the autonomous positioning of satellite constellations are presented. The observability of the pulsar-based measurement model is then shown. Second, the autonomous positioning algorithms, including measurement models and orbital dynamics models, are formulated using an unscented Kalman filter to estimate the position vectors of satellites. Finally, the feasibility of the proposed measurement scheme compared

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Bao, Yiwei, Yang Chen, and Siming Liu. "Is PSR J0855−4644 responsible for the 1.4 TeV electron spectral bump hinted by DAMPE?" Monthly Notices of the Royal Astronomical Society 500, no. 4 (2020): 4573–77. http://dx.doi.org/10.1093/mnras/staa3311.

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ABSTRACT DAMPE observation on the cosmic ray electron spectrum hints a narrow excess at ∼1.4 TeV. Although the excess can be ascribed to dark matter particles, pulsars and pulsar wind nebulae are believed to be more natural astrophysical origins: electrons injected from nearby pulsars at their early ages can form a bump-like feature in the spectrum due to radiative energy losses. In this paper, with a survey of nearby pulsars, we filter out four pulsars that may have notable contributions to ∼1.4 TeV cosmic ray electrons. Among them, PSR J0855−4644 has a spin-down luminosity more than 50 times

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47

Rangelov, Blagoy, Hui Yang, Brice Williams, Oleg Kargaltsev, Jeremy Hare, and Kean Martinic. "Chandra X-Ray Observatory Observations of 13 Fermi LAT Sources." Astrophysical Journal 961, no. 1 (2024): 26. http://dx.doi.org/10.3847/1538-4357/ad09da.

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Abstract In the latest data release from the Fermi Gamma-ray Space Telescope (the 4th Fermi LAT 14 yr Catalog, or 4FGL), more than 50% of the Galactic sources are yet to be identified. We observed 13 unidentified Fermi LAT sources with the Chandra X-Ray Observatory to explore their nature. We report the results of the classification of X-ray sources in the fields of these γ-ray sources and discuss the implications for their nature. We use multiwavelength (MW) data for a machine-learning classification, accompanied by a more detailed spectral/variability analysis for brighter sources. Eight 4FG

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Meliani, M. T. "A Catalogue of X-ray Sources in the Sky Region between δ = −73° and δ = +27°". Publications of the Astronomical Society of Australia 16, № 2 (1999): 175–205. http://dx.doi.org/10.1071/as99175.

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AbstractThis Catalogue lists coordinates, X-ray fluxes in different energy ranges, magnitudes and colour indices, optical counterparts, orbital periods of binaries, pulsar periods and other characteristics of 226 X-ray sources (HMXBs, LMXBs, pulsars and galaxies) between δ = −73° and δ = +27°.

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Melikidze, George I., and Janusz Gil. "Surface magnetic fields in pulsars." Proceedings of the International Astronomical Union 4, S259 (2008): 131–32. http://dx.doi.org/10.1017/s1743921309030324.

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AbstractObservations of hot-spot thermal X-ray emission from radio pulsars implicate that surface magnetic field (SMF) at the polar cap is much stronger than the conventional dipolar component estimated from the pulsar spin-down. This strongly suggests that SMF is dominated by the crust anchored small scale magnetic field. We present the observed values of black body temperature and bolometric luminosity of X-ray emission from hot polar caps of a number of pulsars. In all cases the inferred value of SMF is close to 1014 G.

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Hare, Jeremy, Igor Volkov, George G. Pavlov, Oleg Kargaltsev, and Simon Johnston. "Precise Timing and Phase-resolved Spectroscopy of the Young Pulsar J1617–5055 with NuSTAR." Astrophysical Journal 923, no. 2 (2021): 249. http://dx.doi.org/10.3847/1538-4357/ac30e2.

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Abstract We report on a Nuclear Spectroscopic Telescope Array (NuSTAR) observation of the young, energetic pulsar PSR J1617–5055. Parkes Observatory 3 GHz radio observations of the pulsar (taken about 7 yr before the NuSTAR observations) are also reported here. NuSTAR detected pulsations at a frequency of f ≈ 14.4 Hz (P ≈ 69.44 ms) and, in addition, the observation was long enough to measure the source’s frequency derivative, f ̇ ≈ − 2.8 × 10 − 11 Hz s−1. We find that the pulsar shows one peak per period at both hard X-ray and radio wavelengths, but that the hard X-ray pulse is broader (having

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