J/MNRAS/468/4735ivo://CDS.VizieR/J/MNRAS/468/4735doi:10.26093/cds/vizier.74684735CDSLipunova G.V.Malanchev K.L.2024-08-17T20:18:50Z2017-08-08T16:37:58ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fraccretionx-ray-binary-starsx-ray-sourcesWe 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 C_irr_, 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 {alpha}~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 C_irr_~(2-3)x10^-4^, the resulting {alpha} lie in the interval 0.5-1.5 for the black hole masses in the range 6-10M_{sun}_, while the radius of the ionized disc is variable and controlled by irradiation. For very weak irradiation, C_irr_<1.5x10^-4^, the burst decline develops as in normal outbursts of dwarf novae with {alpha}~0.08-0.32. The optical data indicate that C_irr_ 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 {alpha} 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 {alpha} in X-ray novae using dM(t)/dt.2017MNRAS.468.4735Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/468/4735CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/468/4735https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/468/4735http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/468/4735https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/468/4735https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/468/4735http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/468/4735GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-raydefaultJ/MNRAS/468/4735/figure1Evolution of spectral parameters of 4U 1543-47 during the 2002 outburstObsIDObservation ID (1)meta.id;obscharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinttbeginObservation start (Julian date)stime.epochdoubletendObservation end (Julian date)stime.epochdoublechi2Chi-square of the spectral fit (2)stat.fit.param;meta.modelledfloatdofNumber of degrees of freedom of the spectral fit (3)meta.numberintFDisc-minLower boundary of 1-sigma confidence interval on the disc flux (4)mW.m**-2phot.flux;em.X-raydoubleFDisc-maxUpper boundary of 1-sigma confidence interval on the disc flux (4)mW.m**-2phot.flux;em.X-raydoubleFTot-minLower boundary of 1-sigma confidence interval on the total flux (5)mW.m**-2phot.flux;em.X-raydoubleFTot-maxUpper boundary of 1-sigma confidence interval on the total flux (5)mW.m**-2phot.flux;em.X-raydoubleGammaBest-fit value of the photon power law index in the spectral component simplmeta.code;phys.luminosity;meta.modelleddoubleb_GammaLower boundary of 1-sigma confidence interval for Gammastat.fit.paramdoubleB_GammaUpper boundary of 1-sigma confidence interval for Gammastat.fit.paramdoubleFracSctrBest-fit value of the scattered fraction in the spectral component simplstat.fit.paramdoubleb_FracSctrLower boundary of 1-sigma confidence interval for FracSctrstat.fit.paramdoubleB_FracSctrUpper boundary of 1-sigma confidence interval for FracSctrstat.fit.paramdoubledotMBest-fit value of the mass accretion rate of the disc in the spectral component kerrbb1e+18g.s**-1arith.rate;phys.mass;meta.modelleddoubleb_dotMLower boundary of 1-sigma confidence interval for dotM1e+18g.s**-1stat.fit.paramdoubleB_dotMUpper boundary of 1-sigma confidence interval for dotM1e+18g.s**-1stat.fit.paramdoubledistBest-fit value of the distance in the spectral component kerrbb (6)kpcpos.distancedoubleb_dist? Lower boundary of 1-sigma confidence interval for dist (6)kpcstat.fit.paramdoublenullableB_dist? Upper boundary of 1-sigma confidence interval for dist (6)kpcstat.fit.paramdoublenullableLineEBest-fit value of the line energy in the spectral component laorkeVphys.energy;spect.line;meta.modelleddoubleb_LineE? Lower boundary of 1-sigma confidence interval for LineEkeVstat.fit.paramdoublenullableB_LineE? Upper boundary of 1-sigma confidence interval for LineEkeVstat.fit.paramdoublenullablenormBest-fit value of the photon flux in the spectral component laorph.cm**-2.s**-1phot.flux;meta.modelleddoubleb_norm? Lower boundary of 1-sigma confidence interval for normph.cm**-2.s**-1stat.fit.paramdoublenullableB_normUpper boundary of 1-sigma confidence interval for normph.cm**-2.s**-1stat.fit.paramdoubleedgeEBest-fit value of the threshold energy in the spectral component smedgekeVem.energydoubleb_edgeE? Lower boundary of 1-sigma confidence interval for edgeEkeVstat.fit.paramdoublenullableB_edgeEUpper boundary of 1-sigma confidence interval for edgeEkeVstat.fit.paramdoubleMaxTauBest-fit value of the maximum absorption factor at threshold in the spectral component smedgestat.fit.paramdoubleb_MaxTau? Lower boundary of 1-sigma confidence interval for MaxTaustat.fit.paramdoublenullableB_MaxTauUpper boundary of 1-sigma confidence interval for MaxTaustat.fit.paramdouble