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

被引：29
|
作者：
Suleimanov, V. F. [1 ,2 ]
Lipunova, G. V. [3 ]
Shakura, N. I. [3 ]
机构：
[1] Eberhard Karls Univ Tubingen, Inst Astron & Astrophys, Kepler Ctr Astro & Particle Phys, D-72076 Tubingen, Germany
[2] Kazan VI Lenin State Univ, Kazan 420008, Russia
[3] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Moscow 119992, Russia
来源：
ASTRONOMY & ASTROPHYSICS | 2008年 / 491卷 / 01期
关键词：
binaries: close; X-rays: binaries; stars: individual: Nova Mon 1975; stars: individual: Nova Mus 1991;
D O I：
10.1051/0004-6361:200810155
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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 <= 0.4, 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.
引用
收藏
页码：267 / 277
页数：11
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