2016ApJ...821..104Y


Query : 2016ApJ...821..104Y

2016ApJ...821..104Y - Astrophys. J., 821, 104-104 (2016/April-3)

Testing wind as an explanation for the spin problem in the continuum-fitting method.

YOU B., STRAUB O., CZERNY B., SOBOLEWSKA M., ROZANSKA A., BURSA M. and DOVCIAK M.

Abstract (from CDS):

The continuum-fitting method is one of the two most advanced methods of determining the black hole spin in accreting X-ray binary systems. There are, however, still some unresolved issues with the underlying disk models. One of these issues manifests as an apparent decrease in spin for increasing source luminosity. Here, we perform a few simple tests to establish whether outflows from the disk close to the inner radius can address this problem. We employ four different parametric models to describe the wind and compare these to the apparent decrease in spin with luminosity measured in the sources LMC X-3 and GRS 1915+105. Wind models in which parameters do not explicitly depend on the accretion rate cannot reproduce the spin measurements. Models with mass accretion rate dependent outflows, however, have spectra that emulate the observed ones. The assumption of a wind thus effectively removes the artifact of spin decrease. This solution is not unique; the same conclusion can be obtained using a truncated inner disk model. To distinguish among the valid models, we will need high-resolution X-ray data and a realistic description of the Comptonization in the wind.

Abstract Copyright: © 2016. The American Astronomical Society. All rights reserved.

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

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 Mrk 335 Sy1 00 06 19.5372339024 +20 12 10.617404076   14.19 13.85     ~ 1186 0
2 Mrk 1506 Sy1 04 33 11.0956735296 +05 21 15.619461552   15.72 15.05 10.08   ~ 1934 2
3 X LMC X-3 HXB 05 38 56.6323605504 -64 05 03.317937504   17 17.2     B2.5Ve 649 0
4 X LMC X-1 HXB 05 39 38.8284304464 -69 44 35.531553624   14.8 14.5     O8(f)p 604 2
5 [VV2006] J094534.0+100950 QSO 09 45 33.9892793712 +10 09 50.100934932   18.51 18.16     ~ 54 0
6 NGC 3783 Sy1 11 39 01.7096819040 -37 44 19.009642992   12.46 13.43 11.33 12.1 ~ 1564 0
7 PB 3894 Sy1 12 14 17.6738687784 +14 03 13.182723144   14.46 14.19     ~ 783 0
8 V* IL Lup HXB 15 47 08.2768672752 -47 40 10.284587760     11.96     ~ 453 1
9 2MASX J16332357+4718588 Sy1 16 33 23.5812109560 +47 18 58.936241628   17.77 17.35     ~ 77 1
10 X Nor X-1 LXB 16 34 01.610 -47 23 34.80           ~ 468 0
11 V* V1033 Sco HXB 16 54 00.137 -39 50 44.90   15.20 14.2 16.14   F5IV 1799 1
12 [KRL2007b] 222 LXB 17 09 07.61 -36 24 25.7           ~ 245 1
13 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 675 0
14 [KRL2007b] 353 HXB 19 08 53.080 +09 23 04.84     15.80     ~ 101 0
15 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2463 0
16 HD 226868 HXB 19 58 21.6757355952 +35 12 05.784512688 9.38 9.72 8.91 8.42   O9.7Iabpvar 4137 0

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2022.09.28-02:01:41

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