scholarly journals Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743–322

2018 ◽  
Vol 482 (1) ◽  
pp. 550-559 ◽  
Author(s):  
Zheng Cheng ◽  
Mariano Méndez ◽  
Diego Altamirano ◽  
Aru Beri ◽  
Yanan Wang
Keyword(s):  
Black Hole ◽  
Spectral Analysis ◽  
Periodic Oscillation ◽  
Quasi Periodic Oscillation ◽  
Black Hole Candidate

scholarly journals The determination of the GX 339-4's mass based on its 2010 outburst

2010 ◽  
Vol 6 (S275) ◽  
pp. 327-328
Author(s):  
Tao Chen
Keyword(s):  
Black Hole ◽  
Timing Analysis ◽  
Periodic Oscillation ◽  
Spectral Parameters ◽  
Quasi Periodic Oscillation ◽  
Black Hole Candidate ◽  
Centroid Frequency ◽  
Timing Properties ◽  
The Relationship

AbstractIn this paper we investigate the quasi periodic oscillation (QPO) behavior of the black hole candidate GX 339-4 during its 2010 outburst using RXTE/PCA data. We perform spectral and timing analysis of the observations, where the QPOs are observed. We analyze the relationship between the centroid frequency of QPO and the spectral parameters. The correlation of spectral and timing properties can be used to estimate the mass of black hole with the scaling method. Using this method we estimate a mass of 7.5 ± 0.8 M⊙ of GX 339-4.

scholarly journals A detailed study on the reflection component for the black hole candidate MAXI J1836−194

2020 ◽  
Vol 493 (2) ◽  
pp. 2178-2187
Author(s):  
Yanting Dong ◽  
Javier A García ◽  
Zhu Liu ◽  
Xueshan Zhao ◽  
Xueying Zheng ◽  
...  
Keyword(s):  
Black Hole ◽  
Spectral Analysis ◽  
Primary Source ◽  
Ionization State ◽  
X Ray ◽  
Black Hole Candidate ◽  
Reflection Model ◽  
Iron Abundance ◽  
Reflection Component ◽  
Ionization Gradient

ABSTRACT We present a detailed spectral analysis of the black hole candidate MAXI J1836−194. The source was caught in the intermediate state during its 2011 outburst by Suzaku and RXTE. We jointly fit the X-ray data from these two missions using the relxill model to study the reflection component, and a steep inner emissivity profile indicating a compact corona as the primary source is required in order to achieve a good fit. In addition, a reflection model with a lamp-post configuration (relxilllp), which is normally invoked to explain the steep emissivity profile, gives a worse fit and is excluded at 99 per cent confidence level compared to relxill. We also explore the effect of the ionization gradient on the emissivity profile by fitting the data with two relativistic reflection components, and it is found that the inner emissivity flattens. These results may indicate that the ionization state of the disc is not constant. All the models above require a supersolar iron abundance higher than ∼4.5. However, we find that the high-density version of reflionx can describe the same spectra even with solar iron abundance well. A moderate rotating black hole (a* = 0.84–0.94) is consistently obtained by our models, which is in agreement with previously reported values.

scholarly journals Inference on accretion flow properties of XTE J1752-223 during its 2009-10 outburst

2020 ◽  
Vol 493 (2) ◽  
pp. 2452-2462 ◽  
Author(s):  
Kaushik Chatterjee ◽  
Dipak Debnath ◽  
Debjit Chatterjee ◽  
Arghajit Jana ◽  
Sandip K Chakrabarti
Keyword(s):  
Black Hole ◽  
Spectral Analysis ◽  
Low Frequency ◽  
Power Law Model ◽  
Flow Properties ◽  
Advective Flow ◽  
Black Hole Candidate ◽  
Two Component ◽  
Timing Properties ◽  
Spectral States

ABSTRACT Spectral and timing properties of the stellar-mass black hole candidate XTE J1752-223 during its 2009-10 outburst are studied using RXTE PCA data in the 2.5–25 keV energy range. Low frequency quasi-periodic oscillations are seen during outburst. The spectral analysis is done using two types of models: one is the combined disc blackbody plus power-law model and the other is Transonic flow solution based Two Component Advective Flow (TCAF) model. Light-curve profiles and evolution of hardness ratios are studied using MAXI GSC and Swift BAT data. Based on the evolution of the temporal and the spectral properties, we find that the object evolved through the following spectral states: hard, hard-intermediate, and soft-intermediate/soft. From the TCAF model fitted spectral analysis, we also estimate the probable mass of the black hole in the range of 8.1−11.9 M⊙, and more precisely, the mass appears to be 10 ± 1.9 M⊙.

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