Modeling of non-stationary accretion disks in X-ray novae A 0620–00 and GRS 1124–68 during outburst

Aims. We address the task of modeling soft X-ray and optical light curves of X-ray novae in the high/soft state. Methods. The analytic model of viscous evolution of an externally truncated accretion alpha-disk is used. Relativistic effects near a Kerr black hole and self-irradiation of an accretion...

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Published in:Astronomy and astrophysics (Berlin) 2008-11, Vol.491 (1), p.267-277
Main Authors: Suleimanov, V. F., Lipunova, G. V., Shakura, N. I.
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Language:English
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description Aims. We address the task of modeling soft X-ray and optical light curves of X-ray novae in the high/soft state. Methods. The analytic model of viscous evolution of an externally truncated accretion alpha-disk is used. Relativistic effects near a Kerr black hole and self-irradiation of an accretion disk are taken into account. Results. The model is applied to the outbursts of X-ray nova Monocerotis 1975 (A 0620-00) and X-ray nova Muscae 1991 (GRS 1124-68). Comparison of observational data with the model yields constraints on the angular momentum (the Kerr parameter) of the black holes in A 0620-00 and GRS 1124-68: 0.3-0.6 and leq0.4, and on the viscosity parameter alpha of the disks: 0.7-0.95 and 0.55-0.75. We also conclude that the accretion disks should have an effective geometrical thickness 1.5-2 times greater than the theoretical value of the distance between the photometric layers.
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title Modeling of non-stationary accretion disks in X-ray novae A 0620–00 and GRS 1124–68 during outburst
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