scholarly journals The nature of X-ray spectral variability in SWIFT J2127.4+5654

2018 ◽  
Vol 480 (3) ◽  
pp. 3412-3423
Author(s):  
E S Kammoun ◽  
I E Papadakis
Keyword(s):  
Spectral Variability ◽  
X Ray

scholarly journals X-ray Spectral Evolution of High Energy Peaked Blazars

Galaxies ◽  
2020 ◽  
Vol 8 (3) ◽  
pp. 62
Author(s):  
Haritma Gaur
Keyword(s):  
High Energy ◽  
Energy Interval ◽  
Spectral Studies ◽  
Parabolic Model ◽  
Spectral Evolution ◽  
Spectral Variability ◽  
Spectral Parameters ◽  
X Ray ◽  
Wide Energy ◽  
Energy Dependent

The synchrotron hump of the high energy peaked blazars generally lies in the 0.1–10 keV range and such sources show extreme flux and spectral variability in X-ray bands. Various spectral studies showed that the X-ray spectra of high energy peaked blazars are curved and better described by the log-parabolic model. The curvature is attributed to the energy dependent statistical acceleration mechanism. In this work, we review the X-ray spectral studies of high energy peaked blazars. It is found that the log-parabolic model well describes the spectra in a wide energy interval around the peak. The log-parabolic model provides the possibility of investigating the correlation between the spectral parameters derived from it. Therefore, we compiled the studies of correlations between the various parameters derived from the log-parabolic model and their implications to describe the variability mechanism of blazars.

scholarly journals X-ray Variability of the Flare Star CC Eri

1995 ◽  
Vol 151 ◽  
pp. 170-170
Author(s):  
H.C. Pan ◽  
C. Jordan
Keyword(s):  
Binary Star ◽  
Emission Measure ◽  
Quality Data ◽  
Spectral Variability ◽  
High Quality ◽  
High Quality Data ◽  
X Ray ◽  
Spectroscopic Binary ◽  
Two Temperature ◽  
Continuous Temperature

The flare/spotted spectroscopic binary star CC Eri (HD 16157) was observed in the periods 1990 July 9-11 and 1992 January 26-27 with the ROSAT PSPC detector (Pan and Jordan 1995). These high quality data give the first information on the temporal and spectral variability of CC Eri in the X-ray energy band.During the ROSAT observations the X-ray intensity of the source is variable on timescales from a few minutes to several hours. The X-ray luminosity is in the range 2.5 – 6.8 × 1029 erg s−1, which is similar to values found from previous measurements with the Einstein IPC and EXOSAT LE. On 1990 July 10 an X-ray flare-like event was detected with an exponential rise time of about one hour and a decay time of about two hours. The X-ray spectrum of CC Eri can be described by current thermal plasma codes with two temperature components or with a continuous temperature distribution. The spectral results show that plasma at Te ∼ 107 K exists in the corona of CC Eri. We find that the X-ray spectrum is also variable and the variations of the emission measure, and to a lesser extent of the temperature, are correlated with the source intensity.

X-ray luminosity and spectral variability in the Seyfert type I galaxy - PG 2130 + 099

1991 ◽  
Vol 372 ◽  
pp. 49 ◽  
Author(s):  
K. P. Singh ◽  
A. R. Rao ◽  
M. N. Vahia
Keyword(s):  
Type I ◽  
Spectral Variability ◽  
X Ray ◽  
Seyfert Type

Spectral Variability of the X-Ray--bright BL Lacertae Object PKS 2005-489

1995 ◽  
Vol 449 ◽  
pp. 567 ◽  
Author(s):  
Rita M. Sambruna ◽  
C. Megan Urry ◽  
Gabriele Ghisellini ◽  
Laura Maraschi
Keyword(s):  
Spectral Variability ◽  
X Ray ◽  
Bl Lacertae

scholarly journals The unusual broad-band X-ray spectral variability of NGC 1313 X-1 seen with XMM–Newton, Chandra, and NuSTAR

2020 ◽  
Vol 494 (4) ◽  
pp. 6012-6029 ◽  
Author(s):  
D J Walton ◽  
C Pinto ◽  
M Nowak ◽  
M Bachetti ◽  
R Sathyaprakash ◽  
...  
Keyword(s):  
Black Hole ◽  
Broad Band ◽  
High Energy ◽  
Accretion Disc ◽  
Continuum Emission ◽  
Spectral Variability ◽  
Temperature Behaviour ◽  
Temperature Relation ◽  
X Ray ◽  
Constant Area

ABSTRACT We present results from the major coordinated X-ray observing programme on the ULX NGC 1313 X-1 performed in 2017, combining XMM–Newton, Chandra, and NuSTAR, focusing on the evolution of the broad-band (∼0.3–30.0 keV) continuum emission. Clear and unusual spectral variability is observed, but this is markedly suppressed above ∼10–15 keV, qualitatively similar to the ULX Holmberg IX X-1. We model the multi-epoch data with two-component accretion disc models designed to approximate super-Eddington accretion, allowing for both a black hole and a neutron star accretor. With regards to the hotter disc component, the data trace out two distinct tracks in the luminosity–temperature plane, with larger emitting radii and lower temperatures seen at higher observed fluxes. Despite this apparent anticorrelation, each of these tracks individually shows a positive luminosity–temperature relation. Both are broadly consistent with L ∝ T4, as expected for blackbody emission with a constant area, and also with L ∝ T2, as may be expected for an advection-dominated disc around a black hole. We consider a variety of possibilities for this unusual behaviour. Scenarios in which the innermost flow is suddenly blocked from view by outer regions of the super-Eddington disc/wind can explain the luminosity–temperature behaviour, but are difficult to reconcile with the lack of strong variability at higher energies, assuming this emission arises from the most compact regions. Instead, we may be seeing evidence for further radial stratification of the accretion flow than is included in the simple models considered, with a combination of winds and advection resulting in the suppressed high-energy variability.

scholarly journals LONG-TERM X-RAY MONITORING OF LS I +61°303: ANALYSIS OF SPECTRAL VARIABILITY AND FLARES

2011 ◽  
Vol 733 (2) ◽  
pp. 89 ◽  
Author(s):  
Jian Li ◽  
Diego F. Torres ◽  
Shu Zhang ◽  
Yupeng Chen ◽  
Daniela Hadasch ◽  
...  
Keyword(s):  
Spectral Variability ◽  
X Ray

scholarly journals X-ray Flux and Spectral Variability of the TeV Blazars Mrk 421 and PKS 2155-304

Galaxies ◽  
2020 ◽  
Vol 8 (3) ◽  
pp. 64
Author(s):  
Alok C. Gupta
Keyword(s):  
Black Hole ◽  
Time Series Data ◽  
Series Data ◽  
Physical Parameters ◽  
Electromagnetic Spectrum ◽  
Black Hole Mass ◽  
Spectral Variability ◽  
Massive Black Hole ◽  
X Ray ◽  
Northern And Southern Hemispheres

We reviewed X-ray flux and spectral variability properties studied to date by various X-ray satellites for Mrk 421 and PKS 2155-304, which are TeV emitting blazars. Mrk 421 and PKS 2155-304 are the most X-ray luminous blazars in the northern and southern hemispheres, respectively. Blazars show flux and spectral variabilities in the complete electromagnetic spectrum on diverse timescales ranging from a few minutes to hours, days, weeks, months and even several years. The flux and spectral variability on different timescales can be used to constrain the size of the emitting region, estimate the super massive black hole mass, find the dominant emission mechanism in the close vicinity of the super massive black hole, search for quasi-periodic oscillations in time series data and several other physical parameters of blazars. Flux and spectral variability is also a dominant tool to explain jet as well as disk emission from blazars at different epochs of observations.

scholarly journals X-ray burst-induced spectral variability in 4U 1728–34

2017 ◽  
Vol 599 ◽  
pp. A89 ◽  
Author(s):  
J. J. E. Kajava ◽  
C. Sánchez-Fernández ◽  
E. Kuulkers ◽  
J. Poutanen
Keyword(s):  
Spectral Variability ◽  
X Ray

scholarly journals Probing the circumnuclear absorbing medium of the buried AGN in NGC 1068 through NuSTAR observations

2020 ◽  
Vol 492 (3) ◽  
pp. 3872-3884 ◽  
Author(s):  
A Zaino ◽  
S Bianchi ◽  
A Marinucci ◽  
G Matt ◽  
F E Bauer ◽  
...  
Keyword(s):  
Time Scales ◽  
Line Of Sight ◽  
Nuclear Region ◽  
Spectral Variability ◽  
Absorbing Medium ◽  
X Ray ◽  
Innermost Part ◽  
Monitoring Campaign ◽  
Ngc 1068 ◽  
Thick Material

ABSTRACT We present the results of the latest NuSTAR monitoring campaign of the Compton-thick Seyfert 2 galaxy NGC 1068, composed of four ∼50 ks observations performed between 2017 July and 2018 February to search for flux and spectral variability on time-scales from 1 to 6 months. We detect one unveiling and one eclipsing event with time-scales less than 27 and 91 d, respectively, ascribed to Compton-thick material with NH = (1.8 ± 0.8) × 1024 and ≥ (2.4 ± 0.5) × 1024 cm−2 moving across our line of sight. This gas is likely located in the innermost part of the torus or even further inward, thus providing further evidence of the clumpy structure of the circumnuclear matter in this source. Taking advantage of simultaneous Swift–XRT observations, we also detected a new flaring ULX, at a distance d ∼ 30 arcsec (i.e. ∼2 kpc) from the nuclear region of NGC 1068, with a peak X-ray intrinsic luminosity of (3.0 ± 0.4) × 1040 erg s−1 in the 2–10 keV band.

scholarly journals Infrared spectroscopic variability of Cygnus X-3

1999 ◽  
Vol 193 ◽  
pp. 358-359
Author(s):  
Margaret M. Hanson ◽  
Rob P. Fender ◽  
G.G. Pooley
Keyword(s):  
Mass Transfer ◽  
High Resolution ◽  
Ir Spectroscopy ◽  
Spherically Symmetric ◽  
X Rays ◽  
Spectral Variability ◽  
X Ray ◽  
Orbital Phase ◽  
Band Spectra ◽  
Binary Orbit

We present four epochs of high-resolution IR spectroscopy of the peculiar X-ray binary Cygnus X-3. The observations cover quiescent, small flaring and outburst states of the system as defined by radio and X-ray monitoring. The underlying IR spectrum of the source, as observed during radio and X-ray quiescence and small flaring states is one of broad, weak He II and N V emission. Spectral variability in this state is dominated by modulation at the 4.8 hr orbital period of the system. H-band spectra confirm the significant hydrogen depletion of the mass donor. In outburst, the infrared spectrum is dramatically different, with the appearance of very strong twin-peaked He I emission displaying both day-to-day variability and V (iolet) / R(ed) variations with orbital phase. We argue that the most likely explanation appears to be an enhanced stellar wind from the companion. Thus the X-ray and radio outbursts in this system are likely to originate in mass-transfer, and not disc instabilities. We suggest that the wind in Cyg X-3 is significantly flattened in the plane of the binary orbit. This may explain the observed twin-peaked He I features as well as reconcile the large infrared luminosity with the large optical depth to X-rays if Cyg X-3 is embedded in a spherically symmetric wind.

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