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J/MNRAS/468/4735    Spectral evolution of 4U 1543-47 in 2002 (Lipunova+, 2017)

Determination of the turbulent parameter in accretion discs: effects of self-irradiation in 4U 1543-47 during the 2002 outburst. Lipunova G.V., Malanchev K.L. <Mon. Not. R. Astron. Soc., 468, 4735-4747 (2017)> =2017MNRAS.468.4735L (SIMBAD/NED BibCode)
ADC_Keywords: Accretion ; Binaries, X-ray ; X-ray sources Keywords: accretion, accretion discs - methods: numerical - binaries: close - stars: black holes - X-rays: individual: 4U 1543-47 Abstract: We investigate the viscous evolution of the accretion disc in 4U 1543-47, a black hole binary system, during the first 30 d after the peak of the 2002 burst by comparing the observed and theoretical accretion rate evolution dM(t)/dt. The observed dM(t)/dt is obtained from spectral modelling of the archival Proportional Counter Array aboard the RXTE observatory (RXTE/PCA) data. Different scenarios of disc decay evolution are possible depending on a degree of self-irradiation of the disc by the emission from its centre. If the self-irradiation, which is parametrized by factor Cirr, had been as high as ∼5x10-3, then the disc would have been completely ionized up to the tidal radius and the short time of the decay would have required the turbulent parameter α∼3. We find that the shape of the {dot}M(t) curve is much better explained in a model with a shrinking high-viscosity zone. If Cirr~(2-3)x10-4, the resulting α lie in the interval 0.5-1.5 for the black hole masses in the range 6-10M, while the radius of the ionized disc is variable and controlled by irradiation. For very weak irradiation, Cirr<1.5x10-4, the burst decline develops as in normal outbursts of dwarf novae with α∼0.08-0.32. The optical data indicate that Cirr in 4U 1543-47 (2002) was not greater than approximately (3-6)x10-4. Generally, modelling of an X-ray nova burst allows one to estimate α that depends on the black hole parameters. We present the public 1D code FREDDI to model the viscous evolution of an accretion disc. Analytic approximations are derived to estimate α in X-ray novae using dM(t)/dt. Description: Evolution of the spectral parameters obtained from the fitting of the spectral data obtained with RXTE/PCA in the 2.9-25keV energy band. Some spectral parameters are plotted in Figure 1 of the paper. The black hole mass is 9.4 solar masses, the Kerr parameter is 0.4, the disc inclination is 20.7 grad. The spectral fitting is done using XSPEC 12.9.0. The XSPEC spectral model consists of the following spectral components: TBabs((simpl*kerrbb+laor)smedge). Full description of the spectral parameters can be found in Table A1 and Appendix A of the paper. Objects: ------------------------------------------------ RA (2000) DE Designation(s) ------------------------------------------------ 15 47 08.6 -47 40 10 4U 1543-47 = V* IL Lup ------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file figure1.dat 302 58 Evolution of spectral parameters of 4U 1543-47 during the 2002 outburst
Byte-by-byte Description of file: figure1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- ObsID Observation ID (1) 17- 32 F16.8 s tbegin Observation start (Julian date) 34- 49 F16.8 s tend Observation end (Julian date) 51- 57 F7.4 --- chi2 Chi-square of the spectral fit (2) 59- 60 I2 --- dof Number of degrees of freedom of the spectral fit (3) 62- 71 E10.5 mW/m2 FDisc-min Lower boundary of 1-sigma confidence interval on the disc flux (4) 73- 82 E10.5 mW/m2 FDisc-max Upper boundary of 1-sigma confidence interval on the disc flux (4) 84- 93 E10.5 mW/m2 FTot-min Lower boundary of 1-sigma confidence interval on the total flux (5) 95-104 E10.5 mW/m2 FTot-max Upper boundary of 1-sigma confidence interval on the total flux (5) 106-112 F7.5 --- Gamma Best-fit value of the photon power law index in the spectral component simpl 114-120 F7.5 --- b_Gamma Lower boundary of 1-sigma confidence interval for Gamma 122-128 F7.5 --- B_Gamma Upper boundary of 1-sigma confidence interval for Gamma 130-136 F7.5 --- FracSctr Best-fit value of the scattered fraction in the spectral component simpl 138-144 F7.5 --- b_FracSctr Lower boundary of 1-sigma confidence interval for FracSctr 146-152 F7.5 --- B_FracSctr Upper boundary of 1-sigma confidence interval for FracSctr 154-161 F8.5 10+18g/s dotM Best-fit value of the mass accretion rate of the disc in the spectral component kerrbb 163-170 F8.5 10+18g/s b_dotM Lower boundary of 1-sigma confidence interval for dotM 172-179 F8.5 10+18g/s B_dotM Upper boundary of 1-sigma confidence interval for dotM 181-188 F8.5 kpc dist Best-fit value of the distance in the spectral component kerrbb (6) 190-197 F8.5 kpc b_dist ?=99.99 Lower boundary of 1-sigma confidence interval for dist (6) 199-206 F8.5 kpc B_dist ?=99.99 Upper boundary of 1-sigma confidence interval for dist (6) 208-214 F7.5 keV LineE Best-fit value of the line energy in the spectral component laor 216-222 F7.5 keV b_LineE ?=0 Lower boundary of 1-sigma confidence interval for LineE 224-230 F7.5 keV B_LineE ?=0 Upper boundary of 1-sigma confidence interval for LineE 232-238 F7.5 ph/cm2/s norm Best-fit value of the photon flux in the spectral component laor 240-246 F7.5 ph/cm2/s b_norm ?=99.99 Lower boundary of 1-sigma confidence interval for norm 248-254 F7.5 ph/cm2/s B_norm Upper boundary of 1-sigma confidence interval for norm 256-262 F7.5 keV edgeE Best-fit value of the threshold energy in the spectral component smedge 264-270 F7.5 keV b_edgeE ?=99.99 Lower boundary of 1-sigma confidence interval for edgeE 272-278 F7.5 keV B_edgeE Upper boundary of 1-sigma confidence interval for edgeE 280-286 F7.5 --- MaxTau Best-fit value of the maximum absorption factor at threshold in the spectral component smedge 288-294 F7.5 --- b_MaxTau ?=99.99 Lower boundary of 1-sigma confidence interval for MaxTau 296-302 F7.5 --- B_MaxTau Upper boundary of 1-sigma confidence interval for MaxTau
Note (1): Some rows have the same ObsID because an original observation was divided in two parts. Note (2): The XSPEC spectral model consists of the following spectral components: TBabs((simpl*kerrbb+laor)smedge). Full description of the spectral parameters can be found in Table A1 and Appendix A of the paper. Note (3): The number of the degrees of freedom depends on whether the parameter dist of the spectral component kerrbb is fixed or not (see also the caption of Figure 1 in the paper). dof=40 if the distance to the source was estimated during fitting, dof=41 if the distance was fixed. The number of the spectral channels is 49 for all observations. The total number of the spectral model parameters, free and frozen, is 24. Note (4): The model flux before absorption in the energy band 0.05-50 keV of the following spectral model components: (kerrbb+laor)smedge. Note (5): The model flux before absorption in the energy band 0.05-50 keV of the following spectral model components: (simpl*kerrbb+laor)smedge. Note (6): If the lower and upper boundaries of parameter dist are unspecified, this means that the distance was fixed during fitting.
Acknowledgements: Galina V. Lipunova, galja(at)sai.msu.ru
(End) G. Lipunova [Sternberg Astron. Inst. MSU], P. Vannier [CDS] 08-Aug-2017
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