scholarly journals On the Infrared, Optical, and High‐Energy Emission from the Anomalous X‐Ray Pulsar 4U 0142+61

2004 ◽  
Vol 605 (2) ◽  
pp. 840-845 ◽  
Author(s):  
U. Ertan ◽  
K. S. Cheng
Keyword(s):  
High Energy ◽  
X Ray ◽  
Energy Emission ◽  
High Energy Emission

scholarly journals ON THE INTERACTION OF JETS WITH STELLAR WINDS IN MASSIVE X–RAY BINARIES

2010 ◽  
Vol 19 (06) ◽  
pp. 791-796
Author(s):  
MANEL PERUCHO ◽  
VALENTÍ BOSCH-RAMON ◽  
DMITRY KHANGULYAN
Keyword(s):  
Stellar Wind ◽  
Binary Star ◽  
Three Dimensional ◽  
High Energy ◽  
X Ray ◽  
Energy Emission ◽  
Injection Power ◽  
Radio Band ◽  
High Energy Emission ◽  
X Ray Binaries

We present the first three-dimensional simulations of the evolution of a microquasar jet inside the binary star system. The aim is to study the interaction of these jets with the stellar wind from a massive companion and the possible locations of high-energy emission sites. We have simulated two jets with different injection power in order to give a hint on the minimum power required for the jet to escape the system and become visible in larger scales. In the setup, we include a massive star wind filling the grid through which the jet evolves. We show that jets should have powers of the order of 1037 erg s-1 or more in order not to be destroyed by the stellar wind. The jet–wind interaction results in regions in which high-energy emission could be produced. These results imply the possible existence of a population of X–ray binaries undetected in the radio band due to jet disruption inside the region dominated by the stellar wind.

scholarly journals PSR B0656+14: Combined Optical, X-ray & EUV Studies

2000 ◽  
Vol 177 ◽  
pp. 299-300
Author(s):  
Aaron Golden ◽  
Andy Shearer ◽  
Jerry Edelstein
Keyword(s):  
High Energy ◽  
Archival Data ◽  
Polar Cap ◽  
Optical Photometry ◽  
X Ray ◽  
Energy Emission ◽  
High Energy Emission

AbstractPSR B0656+14’s high energy emission is consistent with that of combined magnetospheric and thermal (surface & polar cap) emission. Uncertainties with the radio-derived distance and X-ray instrumentation sensitivities complicate a definitive thermal characterisation however. A re-analysis of combined ROSAT/EUVE archival data in conjunction with integrated & phase-resolved optical photometry is shown to constrain this characterisation.

scholarly journals X-ray Variability of Blazars

2002 ◽  
Vol 19 (1) ◽  
pp. 49-54 ◽  
Author(s):  
Elena Pian
Keyword(s):  
Energy Range ◽  
High Energy ◽  
Space Missions ◽  
Present Review ◽  
Wide Energy Range ◽  
Spectral Variability ◽  
X Ray ◽  
Energy Emission ◽  
Wide Energy ◽  
High Energy Emission

AbstractCritical progress in our understanding of high energy emission from AGN has been determined in the last 10 years by X-ray monitoring campaigns with many space missions, notably ROSAT, ASCA, RXTE, BeppoSAX, and XMM, often in conjunction with observations at other frequencies. The emphasis of the present review is on recent findings about X-ray variability of blazars. Among AGN, these exhibit the largest amplitude variations of the X-ray emission, often well correlated with variations at higher energies (GeV and TeV radiation). The accurate sampling of the X-ray spectra over more than three decades in energy, made possible by the wide energy range of BeppoSAX, has also shown strong spectral variability in blazar active states, suggesting extreme electron energies and leading to the identification of a class of ‘extreme synchrotron’ sources.

scholarly journals Slow motion pulsar wind nebulae

2021 ◽  
Vol 2103 (1) ◽  
pp. 012020
Author(s):  
K P Levenfish ◽  
G A Ponomaryov ◽  
A E Petrov ◽  
A M Bykov ◽  
A M Krassilchtchikov
Keyword(s):  
Time Scales ◽  
Relative Motion ◽  
Slow Motion ◽  
High Energy ◽  
Pulsar Wind Nebulae ◽  
Extra Time ◽  
X Ray ◽  
Energy Emission ◽  
Pulsar Wind ◽  
High Energy Emission

Abstract We show that even the slow (subsonic) motion of pulsar wind nebulae (PWNe) relative to an ambient matter has a significant impact on their observables. The motion changes the appearance of nebulae on X-ray images, comparing to what would be observed for a nebula at rest. Accounting for the relative motion is necessary to avoid misinterpretation of the structure of the nebulae when analyzing their X-ray morphology. The motion also introduces some extra time scales in variability of non-thermal high-energy emission of PWNe and allows to reproduce a number of their structures that are not explained by stationary nebula models.

scholarly journals CORRELATED X-RAY AND VERY HIGH ENERGY EMISSION IN THE GAMMA-RAY BINARY LS I +61 303

2009 ◽  
Vol 706 (1) ◽  
pp. L27-L32 ◽  
Author(s):  
H. Anderhub ◽  
L. A. Antonelli ◽  
P. Antoranz ◽  
M. Backes ◽  
C. Baixeras ◽  
...  
Keyword(s):  
Gamma Ray ◽  
High Energy ◽  
X Ray ◽  
Energy Emission ◽  
Very High Energy ◽  
High Energy Emission ◽  
Very High

scholarly journals The high-energy emission from HD 93129A near periastron

2020 ◽  
Vol 494 (4) ◽  
pp. 6043-6052
Author(s):  
S del Palacio ◽  
F García ◽  
D Altamirano ◽  
R H Barbá ◽  
V Bosch-Ramon ◽  
...  
Keyword(s):  
Magnetic Field ◽  
High Energy ◽  
X Ray ◽  
Energy Emission ◽  
Collision Region ◽  
Upper Limits ◽  
The Galaxy ◽  
Radiative Model ◽  
Γ Ray ◽  
High Energy Emission

ABSTRACT We conducted an observational campaign towards one of the most massive and luminous colliding wind binaries in the Galaxy, HD 93129A, close to its periastron passage in 2018. During this time the source was predicted to be in its maximum of high-energy emission. Here we present our data analysis from the X-ray satellites Chandra and NuSTAR and the γ-ray satellite AGILE. High-energy emission coincident with HD 93129A was detected in the X-ray band up to ∼18 keV, whereas in the γ-ray band only upper limits were obtained. We interpret the derived fluxes using a non-thermal radiative model for the wind-collision region. We establish a conservative upper limit for the fraction of the wind kinetic power that is converted into relativistic electron acceleration, fNT,e < 0.02. In addition, we set a lower limit for the magnetic field in the wind-collision region as BWCR > 0.3 G. We also argue a putative interpretation of the emission from which we estimate fNT,e ≈ 0.006 and BWCR ≈ 0.5 G. We conclude that multiwavelength, dedicated observing campaigns during carefully selected epochs are a powerful tool for characterizing the relativistic particle content and magnetic field intensity in colliding wind binaries.

scholarly journals High Energy Pulsars: Pulses and Populations

1996 ◽  
Vol 160 ◽  
pp. 331-338 ◽  
Author(s):  
Roger W. Romani
Keyword(s):  
High Energy ◽  
Sky Surveys ◽  
X Ray ◽  
Energy Emission ◽  
Emission Models ◽  
Γ Ray ◽  
High Energy Emission

AbstractRecent X-ray and γ-ray observations have detected a number of isolated spin-powered pulsars. Studies of the pulse profiles of these objects are providing a useful guide to the site of the high energy emission. The γ-ray pulses, which are closely tied to the primary population of radiating particles, seem to be an especially useful discriminant between pulsar models. With an understanding of how the pulsar luminosity and beaming factors evolve with spin parameters, pulsar population syntheses can also be used to check the predictions of high energy emission models. In turn, comparison with γ-ray sky surveys constrains the properties of the young pulsar population.

scholarly journals High-energy emission from NGC 5506, the brightest hard X-ray NLS1

2011 ◽  
Author(s):  
Simona Soldi ◽  
Volker Beckmann ◽  
Neil Gehrels ◽  
Sandra De Jong ◽  
Piotr Lubinski
Keyword(s):  
High Energy ◽  
X Ray ◽  
Energy Emission ◽  
High Energy Emission
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