Connections between jet formation and multiwavelength spectral evolution in black hole transients

AbstractMultiwavelength observations are the key to understand conditions of jet formation in Galactic black hole transient (GBHT) systems. By studying radio and optical-infrared evolution of such systems during outburst decays, the compact jet formation can be traced. Comparing this with X-ray spectral and timing evolution we can obtain physical and geometrical conditions for jet formation, and study the contribution of jets to X-ray emission.In this work, first X-ray evolution - jet relation for XTE J1752-223 will be discussed. This source had very good coverage in X-rays, optical, infrared and radio. A long exposure with INTEGRAL also allowed us to study gamma-ray behavior after the jet turns on. We will also show results from the analysis of data from GX 339-4 in the hard state with SUZAKU at low flux levels. The fits to iron line fluorescence emission show that the inner disk radius increases by a factor of >27 with respect to radii in bright states. This result, along with other disk radius measurements in the hard state will be discussed within the context of conditions for launching and sustaining jets.

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Accretion-outflow connection in the outliers of the “universal” radio/X-ray correlation

Proceedings of the International Astronomical Union ◽

10.1017/s174392131001611x ◽

2010 ◽

Vol 6 (S275) ◽

pp. 255-259

Author(s):

M. Coriat ◽

S. Corbel ◽

L. Prat ◽

J. C. A. Miller-Jones ◽

D. Cseh ◽

...

Keyword(s):

Black Hole ◽

Compact Objects ◽

X Rays ◽

X Ray ◽

Black Hole Candidate ◽

Long Term Study ◽

Hard State ◽

Universal Correlation ◽

X Ray Binaries

AbstractIn recent years, numerous efforts have been devoted to unravel the connection between accretion flow and jets in accreting compact objects. Here we report new constraints on these issues, through the long term study of the radio and X-ray behaviour of the black hole candidate H 1743–322. This source is known to be one of the “outliers” of the universal radio/X-ray correlation, i.e. a group of stellar mass accreting black holes displaying fainter radio emission for a given X-ray luminosity, than expected from the correlation. In this work we find, at high X-ray luminosity in the hard state, a tight radio/X-ray correlation with an unusual steep slope of b = 1.38 ± 0.03. This correlation then breaks below ~5 × 10−3LEdd (M/10M⊙)−1 in X-rays and becomes shallower. When compared with radio/X-ray data from other black hole X-ray binaries, we see that the deviant points of H 1743–322 join the universal correlation and seem to follow it at low luminosity. Based on these results, we investigate several hypotheses that could explain both the b ~ 1.4 slope and the transition toward the universal correlation.

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A Study on the Hysteresis Effect and Spectral Evolution in the Mini-Outbursts of Black Hole X-Ray Binary XTE J1550-564

Frontiers in Astronomy and Space Sciences ◽

10.3389/fspas.2021.651661 ◽

2021 ◽

Vol 8 ◽

Author(s):

Ai-Jun Dong ◽

Chang Liu ◽

Kang Ge ◽

Xiang Liu ◽

Qi-Jun Zhi ◽

...

Keyword(s):

Black Hole ◽

State Transition ◽

Hysteresis Effect ◽

Transition Model ◽

Spectral Evolution ◽

X Ray ◽

Photon Count ◽

Hard State ◽

State Transition Model ◽

Spectral State

One normal outburst and three mini-outbursts have been detected by Rossi X-ray Timing Explorer satellite after 2000 in the well-known black hole X-ray binary XTE J1550-564. In this work, we explore the hysteresis effect of the four outbursts, which is a phenomenon that a similar spectral state transition occurs at different luminosity in an outburst of black hole X-ray binary. A q-like track was found in the hardness-intensity diagram of the normal outburst in 2000 but not in the three mini-outbursts that only occur in the Low/Hard state. The results demonstrate that the hysteresis effect is not apparent in the three mini-outbursts and the X-ray spectra are harder than that of the normal outburst at the same photon count rate. Furthermore, the results of the correlation analysis show that the Γ − F2−10keV correlation of mini-outburst maintain negative in the Low/Hard state with the harder spectra than that of the normal outburst at the same X-ray flux. The X-ray spectral evolution can be well-explained by the state-transition model from the Shakura–Sunyaev disk to the advection-dominated accretion flow, which implies that the three mini-outbursts of XTE J1550-564 might originate from a smaller discrete accretion event.

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GRS 1758–258: RXTE Monitoring of a Rare Persistent Hard State Black Hole

Acta Polytechnica ◽

10.14311/1480 ◽

2011 ◽

Vol 51 (6) ◽

Author(s):

M. Obst ◽

K. Pottschmidt ◽

A. Lohfink ◽

J. Wilms ◽

M. Böck ◽

...

Keyword(s):

Black Hole ◽

State Transitions ◽

Spectral Evolution ◽

X Ray ◽

Soft State ◽

Hard State ◽

Long Term Behavior ◽

X Ray Binaries ◽

Black Hole Candidates

GRS 1758–258 is the least studied of the three persistent black hole X-ray binaries in our Galaxy. It is also one of only two known black hole candidates, including all black hole transients, which shows a decrease of its 3-10 keV flux when entering the thermally dominated soft state, rather than an increase.We present the spectral evolution of GRS 1758–258 from RXTE-PCA observations spanning a time of about 11 years from 1996 to 2007. During this time, seven dim soft states are detected. We also consider INTEGRAL monitoring observations of the source and compare the long-term behavior to that of the bright persistent black hole X-ray binary Cygnus X-1. We discuss the observed state transitions in the light of physical scenarios for black hole transitions.

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Electron-positron processes and spectral evolution in black hole accretion disk dynamo models for AGN sources of the cosmic x-ray and gamma ray backgrounds

10.1063/1.34107 ◽

1983 ◽

Author(s):

Darryl Leiter

Keyword(s):

Black Hole ◽

Accretion Disk ◽

Gamma Ray ◽

Spectral Evolution ◽

X Ray ◽

Black Hole Accretion ◽

Electron Positron ◽

Black Hole Accretion Disk ◽

Disk Dynamo ◽

Hole Accretion

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NICER observations reveal that the X-ray transient MAXI J1348−630 is a black hole X-ray binary

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2842 ◽

2020 ◽

Vol 499 (1) ◽

pp. 851-861 ◽

Cited By ~ 1

Author(s):

L Zhang ◽

D Altamirano ◽

V A Cúneo ◽

K Alabarta ◽

T Enoto ◽

...

Keyword(s):

Black Hole ◽

State Transitions ◽

Spectral Evolution ◽

X Ray ◽

Black Hole Candidate ◽

Soft State ◽

Intermediate States ◽

Different Types ◽

Hard State ◽

Timing Properties

ABSTRACT We studied the outburst evolution and timing properties of the recently discovered X-ray transient MAXI J1348−630 as observed with NICER. We produced the fundamental diagrams commonly used to trace the spectral evolution, and power density spectra to study the fast X-ray variability. The main outburst evolution of MAXI J1348−630 is similar to that commonly observed in black hole transients. The source evolved from the hard state (HS), through hard- and soft-intermediate states, into the soft state in the outburst rise, and back to the HS in reverse during the outburst decay. At the end of the outburst, MAXI J1348−630 underwent two reflares with peak fluxes approximately one and two orders of magnitude fainter than the main outburst, respectively. During the reflares, the source remained in the HS only, without undergoing any state transitions, which is similar to the so-called ‘failed outbursts’. Different types of quasi-periodic oscillations (QPOs) are observed at different phases of the outburst. Based on our spectral-timing results, we conclude that MAXI J1348−630 is a black hole candidate.

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X-ray spectral and timing studies of black hole transients in the hard state at low luminosity

10.1063/1.3696221 ◽

2012 ◽

Author(s):

John A. Tomsick ◽

Kazutaka Yamaoka ◽

Emrah Kalemci ◽

Stéphane Corbel ◽

Philip Kaaret ◽

...

Keyword(s):

Black Hole ◽

X Ray ◽

Hard State

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The X-ray/UV ratio in active galactic nuclei: dispersion and variability

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833631 ◽

2018 ◽

Vol 619 ◽

pp. A95 ◽

Cited By ~ 8

Author(s):

E. Chiaraluce ◽

F. Vagnetti ◽

F. Tombesi ◽

M. Paolillo

Keyword(s):

Black Hole ◽

Cosmological Parameters ◽

Multivariate Regression Analysis ◽

Physical Parameters ◽

Distance Modulus ◽

X Rays ◽

Viewing Angle ◽

Black Hole Mass ◽

Intrinsic Variability ◽

X Ray

Context. The well established negative correlation between the αOX spectral slope and the optical/ultraviolet (UV) luminosity, a by-product of the relation between X-rays and optical/UV luminosity, is affected by relatively large dispersion. The main contributors to this dispersion can be variability in the X-ray/UV ratio and/or changes in fundamental physical parameters. Aims. We want to quantify the contribution from variability within single sources (intra-source dispersion) and that from variations of other quantities different from source to source (inter-source dispersion). Methods. We use archival data from the XMM-Newton Serendipitous Source Catalog (XMMSSC) and from the XMM-OM Serendipitous Ultraviolet Source Survey (XMMOM-SUSS3). We select a sub-sample in order to decrease the dispersion of the relation due to the presence of radio-loud and broad absorption line objects, and that due to absorptions in both X-ray and optical/UV bands. We use the structure function (SF) to estimate the contribution from variability to the dispersion. We analyse the dependence of the residuals of the relation on various physical parameters in order to characterise the inter-source dispersion. Results. We find a total dispersion of σ ∼ 0.12 and find that intrinsic variability contributes 56% of the variance of the αOX − LUV relation. If we select only sources with a larger number of observational epochs (≥3) the dispersion of the relation decreases by approximately 15%. We find weak but significant dependencies of the residuals of the relation on black-hole mass and on Eddington ratio, which are also confirmed by a multivariate regression analysis of αOX as a function of UV luminosity and black-hole mass and/or Eddington ratio. We find a weak positive correlation of both the αOX index and the residuals of the αOX − LUV relation with inclination indicators, such as the full width at half maximum (Hβ) and the equivalent width (EW)[OIII], suggesting a weak increase of X-ray/UV ratio with the viewing angle. This suggests the development of new viewing angle indicators possibly applicable at higher redshifts. Moreover, our results suggest the possibility of selecting a sample of objects, based on their viewing angle and/or black-hole mass and Eddington ratio, for which the αOX − LUV relation is as tight as possible, in light of the use of the optical/UV – X-ray luminosity relation to build a distance modulus (DM)-z plane and estimate cosmological parameters.

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