2019A&A...625A..90R


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.18CEST11:52:32

2019A&A...625A..90R - Astronomy and Astrophysics, volume 625A, 90-90 (2019/5-1)

Inclination effects on the X-ray emission of Galactic black-hole binaries.

REIG P. and KYLAFIS N.D.

Abstract (from CDS):


Context. Galactic black-hole X-ray binaries (BHBs) emit a compact, optically thick, mildly relativistic radio jet when they are in hard and hard-intermediate states. In these states, BHBs exhibit a correlation between the time lag of hard with respect to softer photons and the photon index of the power law component that characterizes the X-ray spectral continuum above ∼10keV. The correlation, however, shows large scatter. In recent years, several works have brought to light the importance of taking into account the inclination of the systems to understand the X-ray and radio phenomenology of BHBs.
Aims. Our objective is to investigate the role that the inclination plays on the correlation between the time lag and photon index.
Methods. We obtained RXTE energy spectra and light curves of a sample of BHBs with different inclination angles. We computed the photon index and the time lag between hard and soft photons and performed a correlation and linear regression analysis of the two variables. We also computed energy spectra and light curves of BHBs using the Monte Carlo technique that reproduces the process of Comptonization in the jet. We account for the inclination effects by recording the photons that escape from the jet at different angles. From the simulated light curves and spectra we obtained model-dependent photon index and time lags, which we compared with those obtained from the real data.
Results. We find that the correlation between the time lag and photon index is tight in low-inclination systems and becomes weaker in high-inclination systems. The amplitude of the lags is also larger at low- and intermediate-inclination angles than at high inclination. We also find that the photon index and time lag, obtained from the simulated spectra and light curves, also follow different relationships for different inclination angle ranges. Our jet model reproduces the observations remarkably well. The same set of models that reproduces the correlation for the low-inclination systems, also accounts for the correlation for intermediate- and high-inclination systems fairly well.
Conclusions. The large dispersion observed in the time lag - photon index correlation in BHBs can naturally be explained as an inclination effect. Comptonization in the jet explains the steeper dependence of the lags on the photon index in low- and intermediate-inclination systems than in high-inclination systems.

Abstract Copyright: © ESO 2019

Journal keyword(s): X-rays: binaries - stars: jets - stars: black holes - accretion - accretion disks

Simbad objects: 25

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Number of rows : 25

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 1A 0620-00 HXB 06 22 44.5420315454 -00 20 44.289428950 10.60 11.40 11.2     K3V-K7V 1052 0
2 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 737 0
3 V* BW Cir HXB 13 58 09.700 -64 44 05.80 17.90 18.00 16.9     ~ 202 1
4 MAXI J1543-564 XB* 15 43 17.336 -56 24 48.35           ~ 44 0
5 V* IL Lup HXB 15 47 08.2766679321 -47 40 10.284971214     11.96     ~ 426 1
6 V* V381 Nor HXB 15 50 58.6520652623 -56 28 35.309070422   17.95 16.6     K3III 1062 0
7 X Nor X-1 LXB 16 34 01.610 -47 23 34.80           ~ 438 0
8 [GHJ2008] 3 HXB 16 50 00.980 -49 57 43.60     11.89     K4V 358 0
9 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1751 1
10 MAXI J1659-152 LXB 16 59 01.680 -15 15 28.73           ~ 199 0
11 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1826 0
12 IGR J17177-3656 LXB 17 17 39.0 -36 56 17           ~ 23 0
13 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 631 0
14 AX J1748.0-2829 LXB 17 48 05.060 -28 28 25.80     13.60     ~ 175 0
15 XTE J1752-223 LXB 17 52 15.090 -22 20 32.36           ~ 168 0
16 2MAXI J1753-013 LXB 17 53 28.2897263704 -01 27 06.256526637 15.30 16.73 16.46 16.15 15.64 ~ 302 0
17 [KRL2007b] 312 LXB 18 17 43.537 -33 01 07.80           ~ 143 0
18 MAXI J1836-194 XB* 18 35 43.440 -19 19 10.48           ~ 113 0
19 PBC J1842.3-1124 XB* 18 42 17.45 -11 25 03.9           ~ 21 0
20 V* V406 Vul HXB 18 58 41.580 +22 39 29.40 15.00 15.65 15.31     G5V-K0V 326 0
21 [KRL2007b] 353 HXB 19 08 53.080 +09 23 04.84     15.80     ~ 88 0
22 4U 1907+09 HXB 19 09 37.9 +09 49 49   19.41 16.35 14.40 12.53 O8.5Iab 312 1
23 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2361 0
24 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3997 0
25 V* V404 Cyg HXB 20 24 03.820 +33 52 01.90 14.50 14.20 12.7     K0IV 1125 0

    Equat.    Gal    SGal    Ecl

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2021.04.18-11:52:32

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