Disk accretion onto a black hole at subcritical luminosity.
Disk accretion onto a black hole at subcritical luminosity.
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DOI：
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发表时间：
1977-07
影响因子：
6.5
通讯作者：
G. Bisnovatyi-Kogan;S. Blinnikov
中科院分区：
文献类型：
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作者：
G. Bisnovatyi-Kogan;S. Blinnikov
当总光度L接近Eddington极限L/sub c/时，考虑了辐射压力对吸积盘结构的影响。研究了非旋转黑洞盘辐射场和引力场中粒子的运动。结果表明，当L约等于（0.6 + 1.0）L/sub c/时，盘状吸积被破坏。物质从圆盘的中心部分向无限远处流出。得出的结论是，光度不会明显超过爱丁顿极限。结果表明，当L大于或近似等于0.1 L/sub c/时，圆盘中心区域上层的等离子体被加热到约10/sup 9/ K，与标准理论相比，圆盘变厚。辐射力可以产生大约100g的磁场B。对流是圆盘中心沿z轴方向的主要能量传递机制。对流产生一种声通量，这种声通量在磁盘的上层光学薄层中消散并加热它们。软光子从较低的层到较热的层的复合化和变化的吸积速率可以解释天鹅座X-1的光谱和x射线发射的变化。«少
The influence of radiation pressure on the structure of accretion disk is considered when the total luminosity L approaches the Eddington limit L/sub c/. The motion of particles in the disk radiation field and gravitational field of a nonrotating black hole was investigated. It is shown that the disk accretion is destroyed when L approximately equals (0.6 + 1.0)L/sub c/. Matter outflow from the central parts of the disk to infinity then sets in. It is concluded that the luminosity cannot significantly exceed the Eddington limit. It is shown that for L greater than or approximately equal to 0.1 L/sub c/ the plasma in upper layers of the central region of the disk is heated up to temperatures approximately 10/sup 9/ K, and the disk becomes thicker as compared with the standard theory. The radiative force can generate magnetic fields B approximately 100 Gs. Convection is the main energy transfer mechanism along Z-coordinate in the central parts of the disk. The convection generates an acoustic flux which dissipates in the upper, optically thin layers of the disk and heats them. The comptonization of soft photons going from lower layers to the hot upper layers and variable accretion rate may explainmore » the spectrum and variations of X-ray emission of the Cyg X-1.« less