scholarly journals Accretion flow dynamics during the evolution of timing and spectral properties of GX 339-4 during its 2010–11 outburst

2012 ◽  
Vol 542 ◽  
pp. A56 ◽  
Author(s):  
A. Nandi ◽  
D. Debnath ◽  
S. Mandal ◽  
S. K. Chakrabarti
Keyword(s):  
Spectral Properties ◽  
Flow Dynamics ◽  
Accretion Flow

scholarly journals ACCRETION FLOW DYNAMICS OF MAXI J1659-152 FROM THE SPECTRAL EVOLUTION STUDY OF ITS 2010 OUTBURST USING THE TCAF SOLUTION

2015 ◽  
Vol 803 (2) ◽  
pp. 59 ◽  
Author(s):  
Dipak Debnath ◽  
Aslam Ali Molla ◽  
Sandip K. Chakrabarti ◽  
Santanu Mondal
Keyword(s):  
Flow Dynamics ◽  
Spectral Evolution ◽  
Accretion Flow ◽  
Evolution Study

scholarly journals Dynamics of Low Luminosity Accretion onto Neutron Stars: Spherically Symmetric Models

1997 ◽  
Vol 163 ◽  
pp. 824-825
Author(s):  
John C. L. Wang ◽  
Ralph S. Sutherland
Keyword(s):  
Interstellar Medium ◽  
Neutron Stars ◽  
Flow Dynamics ◽  
Stellar Surface ◽  
Spherically Symmetric ◽  
Atomic Processes ◽  
High Luminosity ◽  
Strongly Coupled ◽  
Accretion Flow ◽  
The Galaxy

The ~ 108−109 old neutron stars in the Galaxy may be undergoing low luminosity accretion from the interstellar medium (Ostriker et al. 1970; Shvartsman 1971). It was first recognized by Shvartsman (1971) that the accretion induced radiation from the stellar surface can heat the infalling material, which in turn inhibits further accretion. This preheating instability has been studied in detail in the high luminosity regime where equilibrium ionization and heating holds (e.g., Buff & McCray 1974; Ostriker et al. 1976; Cowie et al. 1978). In the low luminosity regime, however, dynamical timescales are typically much shorter than atomic timescales so the accretion flow dynamics is strongly coupled to non-equilibrium (NEQ) atomic processes (cf. Blaes et al. 1995).

scholarly journals THE EFFECTS OF ACCRETION FLOW DYNAMICS ON THE BLACK HOLE SHADOW OF SAGITTARIUS A*

2016 ◽  
Vol 831 (1) ◽  
pp. 4 ◽  
Author(s):  
Hung-Yi Pu ◽  
Kazunori Akiyama ◽  
Keiichi Asada
Keyword(s):  
Black Hole ◽  
Flow Dynamics ◽  
Accretion Flow ◽  
Sagittarius A

scholarly journals ACCRETION FLOW DYNAMICS OF MAXI J1836-194 DURING ITS 2011 OUTBURST FROM TCAF SOLUTION

2016 ◽  
Vol 819 (2) ◽  
pp. 107 ◽  
Author(s):  
Arghajit Jana ◽  
Dipak Debnath ◽  
Sandip K. Chakrabarti ◽  
Santanu Mondal ◽  
Aslam Ali Molla
Keyword(s):  
Flow Dynamics ◽  
Accretion Flow

scholarly journals Impact of Accretion Flow Dynamics on Gas-dynamical Black Hole Mass Estimates

2019 ◽  
Vol 882 (2) ◽  
pp. 82 ◽  
Author(s):  
Britton Jeter ◽  
Avery E. Broderick ◽  
B. R. McNamara
Keyword(s):  
Black Hole ◽  
Flow Dynamics ◽  
Black Hole Mass ◽  
Accretion Flow

scholarly journals Accretion flow dynamics during 1999 outburst of XTE J1859+226—modeling of broadband spectra and constraining the source mass

2018 ◽  
Vol 363 (5) ◽  
Author(s):  
Anuj Nandi ◽  
S. Mandal ◽  
H. Sreehari ◽  
D. Radhika ◽  
Santabrata Das ◽  
...  
Keyword(s):  
Flow Dynamics ◽  
Accretion Flow ◽  
Source Mass

scholarly journals EVIDENCE OF VARIATION OF THE ACCRETION FLOW GEOMETRY IN GRS 1915 + 105 FROM IXAE AND RXTE DATA

2011 ◽  
Vol 20 (11) ◽  
pp. 2281-2289 ◽  
Author(s):  
PARTHA SARATHI PAL ◽  
SANDIP K. CHAKRABARTI ◽  
ANUJ NANDI
Keyword(s):  
Light Curve ◽  
Power Law ◽  
Spectral Properties ◽  
Accretion Rate ◽  
Light Curves ◽  
Accretion Flow ◽  
Flow Geometry ◽  
Photon Component

The Galactic microquasar GRS 1915 + 105 exhibits various types of light curves. There is, however, no understanding of when a certain type of light curve will be exhibited and only in a handful of cases, the transitions from one type to another have actually been observed. We study the detailed spectral properties in these cases to show that different classes have different ratio of the power-law photon and the blackbody photon. Since the power-law photons are from the Compton cloud, and the intensity of the power-law photon component depends on the degree of interception of the soft photons by the Compton cloud, we conclude that not only the accretion rate, but the accretion flow geometry must also change during a class transition.

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