2018MNRAS.479.1210G


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.16CEST11:25:20

2018MNRAS.479.1210G - Mon. Not. R. Astron. Soc., 479, 1210-1220 (2018/September-1)

Signature of Two-Component Advective Flow in several Black Hole candidates obtained through time-of-arrival analysis of RXTE/ASM Data.

GHOSH A. and CHAKRABARTI S.K.

Abstract (from CDS):

We study several Galactic black hole candidates using long-time Rossi X-ray Timing Explorer/All Sky Monitor X-ray data to search for telltale signatures of differences in viscous timescales in the two components used in the two-component advective flow paradigm. In high-mass X-ray binaries (HMXBs) mainly winds are accreted. This nearly inviscid and dominant sub-Keplerian flow falls almost freely towards the black hole. A standard Keplerian disc can form out of this sub-Keplerian matter in presence of a significant viscosity and could be small in size. However, in low-mass X-ray binaries (LMXBs), highly viscous and larger Keplerian accretion disc is expected to form inside the sub-Keplerian disc due to the Roche lobe overflow. Due to two viscous timescales in these two components, it is expected to have a larger lag between the times of arrival of these components in LMXBs than that in HMXBs. Direct cross-correlation between the photon fluxes will not reveal this lag since they lack linear dependence, however, they are coupled through the viscous processes which bring in both matter. To quantify the aforesaid time lag, we introduce an index (Θ), which is a proxy of the usual photon index (Γ). Thus, when Θ, being dynamically responsive to both fluxes, is considered as a reference, the arrival time lag between the two fluxes in LMXBs is found to be much larger than that in HMXBs. Our result establishes the presence of two dynamical components in accretion and shows that the Keplerian disc size indeed is smaller in HMXBs as compared to that in LMXBs.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): accretion, accretion discs - viscosity - X-rays: binaries - Outbursts - Cyg X-1, GRS 1915+105

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 V* IL Lup HXB 15 47 08.2766679321 -47 40 10.284971214     11.96     ~ 426 1
2 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1062 0
3 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
4 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1751 1
5 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1826 0
6 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 642 1
7 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 366 1
8 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2361 0
9 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3997 0
10 V* V1521 Cyg HXB 20 32 25.78 +40 57 27.9           WN4/5-6/7 1804 2

    Equat.    Gal    SGal    Ecl

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2021.04.16-11:25:20

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