2013ApJ...769...16R


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.12CEST15:16:05

2013ApJ...769...16R - Astrophys. J., 769, 16 (2013/May-3)

A Swift survey of accretion onto stellar-mass black holes.

REYNOLDS M.T. and MILLER J.M.

Abstract (from CDS):

We present a systemic analysis of all of the stellar-mass black hole binaries (confirmed and candidate) observed by the Swift observatory up to 2010 June. The broad Swift bandpass enables a trace of disk evolution over an unprecedented range in flux and temperature. The final data sample consists of 476 X-ray spectra containing greater than 100 counts, in the 0.6-10 keV band. This is the largest sample of high-quality CCD spectra of accreting black holes published to date. In addition, strictly simultaneous data at optical/UV wavelengths are available for 255 (54%) of these observations. The data are modeled with a combination of an accretion disk and a hard spectral component. For the hard component we consider both a simple power-law model and a thermal Comptonization model. An accretion disk is detected at greater than the 5σ confidence level in 61% of the observations. Light curves and color-color diagrams are constructed for each system. Hardness-luminosity and disk fraction-luminosity diagrams are constructed and are observed to be consistent with those typically observed by RXTE, noting the sensitivity below 2 keV provided by Swift. The observed spectra have an average luminosity of ∼1% Eddington, though we are sensitive to accretion disks down to a luminosity of 10–3 LEdd. Thus, this is also the largest sample of such cool accretion disks studied to date. The accretion disk temperature distribution displays two peaks consistent with the classical hard and soft spectral states, with a smaller number of disks distributed between these. The distribution of inner disk radii is observed to be continuous regardless of which model is used to fit the hard continua. There is no evidence for large-scale truncation of the accretion disk in the hard state (at least for Lx ≳ 10–3 L Edd), with all of the accretion disks having radii ≲ 40 Rg. Plots of the accretion disk inner radius versus hardness ratio reveal the disk radius to be decreasing as the spectrum hardens, i.e., enters the hard state. This is in contrast to expectations from the standard disk truncation paradigm and points toward a contribution from spectral hardening. The availability of simultaneous X-ray and optical/UV data for a subset of observations facilitates a critical examination of the role of disk irradiation via a modified disk model with a variable emissivity profile (i.e., T(r)∝r –p ). The broadband spectra (X-ray-optical/UV) reveal irradiation of the accretion disk to be an important effect at all luminosities sampled herein, i.e., p ≲ 0.75 for luminosities ≳ 10–3 LEdd. The accretion disk is found to dominate the UV emission irrespective of the assumed hard spectral component. Overall, we find the broadband soft-state spectra to be consistent with an irradiated accretion disk plus a corona, but we are unable to make conclusive statements regarding the nature of the hard-state accretion flow (e.g., ADAF/corona versus jet). Finally, the Swift data reveal a relation between the flux emitted by the accretion disk and that emitted by the corona, for this sample of stellar-mass black holes, that is found to be in broad agreement with the observed disk-corona relationship in Seyfert galaxies, suggesting a scale invariant coupling between the accretion disk and the corona.

Abstract Copyright:

Journal keyword(s): accretion, accretion disks - black hole physics - X-rays: binaries

Simbad objects: 32

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Number of rows : 32

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME IC 10 X-1 HXB 00 20 29.09 +59 16 51.9           ~ 148 0
2 NAME NGC 300 X-1 HXB 00 55 09.990 -37 42 12.16     22.44     WNE 103 1
3 NAME M33 X-7 HXB 01 33 34.13 +30 32 11.3 17.50 18.80 18.70     O 127 2
4 V* V518 Per HXB 04 21 42.7231318463 +32 54 26.936934166 13.00 13.50 13.2     M4.5V 620 1
5 X LMC X-3 HXB 05 38 56.6325045489 -64 05 03.321118015   17 17.2     B2.5Ve 630 0
6 X LMC X-1 HXB 05 39 38.8285930597 -69 44 35.533031148   14.8 14.5     O8(f)p 560 2
7 V* KV UMa HXB 11 18 10.7922353051 +48 02 12.319175505     12.25     K5V-M1V 721 0
8 NGC 4395 Sy2 12 25 48.8639154223 +33 32 48.694684028 10.84 10.54 10.11 9.98   ~ 994 1
9 V* BW Cir HXB 13 58 09.700 -64 44 05.80 17.90 18.00 16.9     ~ 192 1
10 SWIFT J1539.2-6227 LXB 15 39 11.963 -62 28 02.30           ~ 20 0
11 X Nor X-1 LXB 16 34 01.610 -47 23 34.80           ~ 418 0
12 XTE J1652-453 XB* 16 52 20.330 -45 20 39.99           ~ 41 1
13 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1701 1
14 V* V821 Ara HXB 17 02 49.3810714542 -48 47 23.163091737 16.20 16.30 15.5     ~ 1764 0
15 [KRL2007b] 222 LXB 17 09 07.61 -36 24 25.7           ~ 209 1
16 [KRL2007b] 224 HX? 17 09 46.124 -36 27 57.31   21.16       ~ 45 0
17 NAME Great Annihilator LXB 17 43 54.83 -29 44 42.6           ~ 638 1
18 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11542 0
19 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 599 0
20 [CHM2006] Candidate 1b LXB 17 49 38.039 -28 21 17.50           ~ 65 0
21 RX J1749.8-3312 LXB 17 49 48.940 -33 12 11.60           ~ 48 0
22 XTE J1752-223 LXB 17 52 15.090 -22 20 32.36           ~ 159 0
23 2MAXI J1753-013 LXB 17 53 28.2897263704 -01 27 06.256526637 15.30 16.73 16.46 16.15 15.64 ~ 280 0
24 2XMM J180112.4-254436 LXB 18 01 12.40 -25 44 36.1           ~ 361 1
25 [KRL2007b] 312 LXB 18 17 43.537 -33 01 07.80           ~ 138 0
26 XTE J1818-245 LXB 18 18 24.430 -24 32 17.96           ~ 34 0
27 V* V4641 Sgr HXB 18 19 21.6342721789 -25 24 25.849323550     13.654   13.092 B9III 386 1
28 PBC J1842.3-1124 XB* 18 42 17.45 -11 25 03.9           ~ 17 0
29 INTREF 948 LXB 18 56 42.920 +05 18 34.30           ~ 41 0
30 Granat 1915+105 LXB 19 15 11.54938 +10 56 44.7585           ~ 2285 0
31 HD 226868 HXB 19 58 21.6758193269 +35 12 05.782512305 9.38 9.72 8.91 8.42   O9.7Iabpvar 3925 0
32 V* V1408 Aql LXB 19 59 24.0077707935 +11 42 29.856991417 18.40 18.97 18.95 18.70 18.66 ~ 167 0

    Equat.    Gal    SGal    Ecl

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2020.07.12-15:16:05

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