scholarly journals Probing Supercritical Accretion in Ultraluminous X-ray Source M82 X-1 by means of X-ray Spectral Evolution Analysis

2020 ◽  
Vol 240 ◽  
pp. 07005
Author(s):  
Izatul Hafizah ◽  
Kiki Vierdayanti
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Accretion Rate ◽  
Spectral Evolution ◽  
X Ray ◽  
Mass Accretion Rate ◽  
Blackbody Model ◽  
Chi Squared ◽  
Dominant State ◽  
Black Hole Binary

We analyze the spectral evolution of ultraluminous X-ray source (ULX) M82 X-1 by means of spectral fitting. We use selected Swift/XRT data in 2014 and 2015. The flux of M82 X-1 increased by a factor of 2-3 from 2014 to 2015. Most of the data in 2015 show greater dominance of hard component than those of 2014. Due to moderate signal-to-noise ratio, we only fit each spectrum with power-law and disk blackbody model separately. The data in 2014 are better fitted with powerlaw model based on the value of reduced-chi squared. On the other hand, both powerlaw and diskbb models showed comparable re- duced chi-squared value for the data in 2015. We found that the range of spectral index for 2014 data is 1.65 < Γ < 2.08 and for 2015 data is 1.02 < Γ < 1.95 from the powerlaw model, resembling the range for that of black hole binary system at low mass accretion rate. We obtained higher innermost disk temper- ature from the disk blackbody model, 1.20 keV < Tin < 3.63 keV, compared to that of black hole binary system in the thermal state. The calculated innermost radius of the disk, Rin, varies between 0.99 to 4.89 RS assuming 10 M0 black hole which indicates that the spectral state is not in thermal dominant state but rather we suspect that M82 X-1 exhibits greater mass accretion rate than that of the thermal dominant state.

Improved Parameters for the Black Hole Binary System X-Ray Nova MUSCAE 1991

1996 ◽  
Vol 468 ◽  
pp. 380 ◽  
Author(s):  
Jerome A. Orosz ◽  
Charles D. Bailyn ◽  
Jeffrey E. McClintock ◽  
Ronald A. Remillard
Keyword(s):  
Black Hole ◽  
Binary System ◽  
X Ray ◽  
Black Hole Binary

scholarly journals MHD Accretion Disk Winds: The Key to AGN Phenomenology?

Galaxies ◽  
2019 ◽  
Vol 7 (1) ◽  
pp. 13 ◽  
Author(s):  
Demosthenes Kazanas
Keyword(s):  
Black Hole ◽  
Accretion Disk ◽  
Accretion Disks ◽  
Mass Flux ◽  
Accretion Rate ◽  
Compact Object ◽  
Mass Scale ◽  
Observational Constraints ◽  
X Ray ◽  
Mass Accretion Rate

Accretion disks are the structures which mediate the conversion of the kinetic energy of plasma accreting onto a compact object (assumed here to be a black hole) into the observed radiation, in the process of removing the plasma’s angular momentum so that it can accrete onto the black hole. There has been mounting evidence that these structures are accompanied by winds whose extent spans a large number of decades in radius. Most importantly, it was found that in order to satisfy the winds’ observational constraints, their mass flux must increase with the distance from the accreting object; therefore, the mass accretion rate on the disk must decrease with the distance from the gravitating object, with most mass available for accretion expelled before reaching the gravitating object’s vicinity. This reduction in mass flux with radius leads to accretion disk properties that can account naturally for the AGN relative luminosities of their Optical-UV and X-ray components in terms of a single parameter, the dimensionless mass accretion rate. Because this critical parameter is the dimensionless mass accretion rate, it is argued that these models are applicable to accreting black holes across the mass scale, from galactic to extragalactic.

scholarly journals The X-Ray Outburst of PG 1553+113: A Precession Effect of Two Jets in the Supermassive Black Hole Binary System

2021 ◽  
Vol 922 (2) ◽  
pp. 222
Author(s):  
Shifeng Huang ◽  
Hongxing Yin ◽  
Shaoming Hu ◽  
Xu Chen ◽  
Yunguo Jiang ◽  
...  
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Light Curve ◽  
Quiescent State ◽  
Black Hole Mass ◽  
X Ray ◽  
Supermassive Black Hole ◽  
System A ◽  
Black Hole Binary ◽  
Two Jets

Abstract Blazar PG 1553+113 is thought to be a host of supermassive black hole binary system. A 2.2 yr quasi-periodicity in the γ-ray light curve was detected, possibly a result of jet precession. Motivated by the previous studies based on the γ-ray data, we analyzed the X-ray light curve and spectra observed during 2012–2020. The 2.2 yr quasi-periodicity might be consistent with the main-flare recurrence in the X-ray light curve. When a weak rebrightening in the γ-ray was observed, a corresponding relatively strong brightening in the X-ray light curve can be identified. The harder-when-brighter tendency in both X-ray main and weak flares was shown, as well as a weak softer-when-brighter behavior for the quiescent state. We explore the possibility that the variability in the X-ray band can be interpreted with two-jet precession scenario. Using the relation between jets and accretion disks, we derive the primary black hole mass ≃3.47 × 108 M ☉ and mass of the secondary one ≃1.40 × 108 M ☉, and their mass ratio ∼0.41.

Testing propagating mass accretion rate fluctuations model PROPFLUC on black hole X-ray binaries

2016 ◽  
Vol 337 (4-5) ◽  
pp. 524-528
Author(s):  
S. Rapisarda ◽  
A. Ingram ◽  
M. van der Klis
Keyword(s):  
Black Hole ◽  
Accretion Rate ◽  
X Ray ◽  
Mass Accretion Rate ◽  
X Ray Binaries

scholarly journals Black Hole Binaries in Quiescence

2016 ◽  
Vol 12 (S324) ◽  
pp. 35-38
Author(s):  
Charles D. Bailyn
Keyword(s):  
Black Hole ◽  
Binary Systems ◽  
Accretion Rate ◽  
Quiescent State ◽  
X Ray ◽  
Black Hole Binaries ◽  
Key Factor ◽  
Black Hole Binary ◽  
Limiting Case ◽  
X Ray Binaries

AbstractI discuss some of what is known and unknown about the behavior of black hole binary systems in the quiescent accretion state. Quiescence is important for several reasons: 1) the dominance of the companion star in optical and IR wavelengths allows the binary parameters to be robustly determined — as an example, we argue that the longer proposed distance to the X-ray source GRO J1655-40 is correct; 2) quiescence represents the limiting case of an extremely low accretion rate, in which both accretion and jets can be observed; 3) understanding the evolution and duration of the quiescent state is a key factor in determining the overall demographics of X-ray binaries, which has taken on a new importance in the era of gravitational wave astronomy.

VLBI OBSERVATIONS OF THE SHORTEST ORBITAL PERIOD BLACK HOLE X-RAY BINARY

2012 ◽  
Vol 08 ◽  
pp. 380-383
Author(s):  
ZSOLT PARAGI ◽  
TOMASO M. BELLONI ◽  
ALEXANDER J. VAN DER HORST ◽  
JAMES MILLER-JONES
Keyword(s):  
Black Hole ◽  
Binary System ◽  
Orbital Period ◽  
X Ray ◽  
Show Evidence ◽  
Multi Wavelength ◽  
Black Hole Binary ◽  
Wavelength Monitoring ◽  
Early Phases ◽  
Extended Emission

The X-ray transient MAXI J1659-152 was discovered by Swift/BAT and it was initially identified as a GRB. Soon its Galactic origin and binary nature were established. There exists a wealth of multi-wavelength monitoring data for this source, providing a great coverage of the full X-ray transition in this candidate black hole binary system. We obtained two epochs of EVN/e-VLBI and four epochs of VLBA data of MAXI J1659-152 which show evidence for some extended emission in the early phases but –against expectations– no major collimated ejecta during the accretion disk state transition. This might be related to the fact that, with a red dwarf donor star, MAXI J1659-152 is the shortest orbital period black hole X-ray binary system.

JET FORMATION IN MICROQUASARS AND ACTIVE GALACTIC NUCLEI: MAGNETIC FIELD LIMITS

2008 ◽  
Vol 17 (10) ◽  
pp. 1931-1937
Author(s):  
M. M. KAUFMAN BERNADÓ ◽  
M. MASSI
Keyword(s):  
Magnetic Field ◽  
Black Hole ◽  
Field Strength ◽  
Magnetic Field Strength ◽  
Accretion Rate ◽  
Plasma Pressure ◽  
X Ray ◽  
Mass Accretion Rate ◽  
Disk Material ◽  
The Magnetic Field

We introduce the use of a well-known parameter, the Alfvén Radius, R A , as a new tool to discern whether an X-ray binary system may undergo a microquasar phase, i.e. ejecting relativistic particles orthogonal to the accretion disk. We study what we call the basic condition, R A /R* = 1 in its dependency on the magnetic field strength and the mass accretion rate. With this basic condition we establish under which combination of parameters any class of accreting neutron stars could become a microquasar instead of confining disk-material down to the magnetic poles and creating the two emitting caps typical for an X-ray pulsar. In the case of black-hole accreting binaries we equate the magnetic field pressure to the plasma pressure in the last stable orbit (i.e. R A /R LSO = 1) and we get upper limits for the magnetic field strength as a function of the mass accretion rate and the black hole mass.

scholarly journals Ultraluminous X-ray sources with flat-topped noise and QPO

2019 ◽  
Vol 486 (2) ◽  
pp. 2766-2779 ◽  
Author(s):  
Kirill Atapin ◽  
Sergei Fabrika ◽  
Maria D Caballero-García
Keyword(s):  
Black Hole ◽  
Power Density ◽  
Root Mean Square ◽  
Accretion Rate ◽  
Mean Square ◽  
Periodic Oscillations ◽  
Simple Interpretation ◽  
X Ray ◽  
Mass Accretion Rate ◽  
Ngc 6946

ABSTRACT We analysed the X-ray power density spectra of five ultraluminous X-ray sources (ULXs) NGC 5408 X-1, NGC 6946 X-1, M 82 X-1, NGC 1313 X-1, and IC 342 X-1 that are the only ULXs that display both flat-topped noise (FTN) and quasi-periodic oscillations (QPOs). We studied the QPO frequencies, fractional root-mean-square (rms) variability, X-ray luminosity, and spectral hardness. We found that the level of FTN is anticorrelated with the QPO frequency. As the frequency of the QPO and brightness of the sources increase, their fractional variability decreases. We propose a simple interpretation using the spherization radius, viscosity time, and α-parameter as basic properties of these systems. The main physical driver of the observed variability is the mass accretion rate that varies ≳3 between different observations of the same source. As the accretion rate decreases the spherization radius reduces and the FTN plus the QPO move towards higher frequencies, resulting in a decrease of the fractional rms variability. We also propose that in all ULXs when the accretion rate is low enough (but still super-Eddington) the QPO and FTN disappear. Assuming that the maximum X-ray luminosity depends only on the black hole (BH) mass and not on the accretion rate (not considering the effects of either the inclination of the super-Eddington disc or geometrical beaming of radiation), we estimate that all the ULXs have about similar BH masses, with the exception of M 82 X-1, which might be 10 times more massive.

scholarly journals X-ray properties of reverberation-mapped AGNs with super-Eddington accreting massive black holes

2019 ◽  
Vol 15 (S356) ◽  
pp. 143-143
Author(s):  
Jaya Maithil ◽  
Michael S. Brotherton ◽  
Bin Luo ◽  
Ohad Shemmer ◽  
Sarah C. Gallagher ◽  
...  
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Accretion Rate ◽  
Time Lags ◽  
Black Hole Mass ◽  
Host Galaxies ◽  
Massive Black Holes ◽  
X Ray ◽  
Photon Index ◽  
The Impact

AbstractActive Galactic Nuclei (AGN) exhibit multi-wavelength properties that are representative of the underlying physical processes taking place in the vicinity of the accreting supermassive black hole. The black hole mass and the accretion rate are fundamental for understanding the growth of black holes, their evolution, and the impact on the host galaxies. Recent results on reverberation-mapped AGNs show that the highest accretion rate objects have systematic shorter time-lags. These super-Eddington accreting massive black holes (SEAMBHs) show BLR size 3-8 times smaller than predicted by the Radius-Luminosity (R-L) relationship. Hence, the single-epoch virial black hole mass estimates of highly accreting AGNs have an overestimation of a factor of 3-8 times. SEAMBHs likely have a slim accretion disk rather than a thin disk that is diagnostic in X-ray. I will present the extreme X-ray properties of a sample of dozen of SEAMBHs. They indeed have a steep hard X-ray photon index, Γ, and demonstrate a steeper power-law slope, ασx.

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