The Jets and and Supercritical Accretion Disk in SS433
The Jets and and Supercritical Accretion Disk in SS433
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SS433 中的喷流和超临界吸积盘
DOI：
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
S. Fabrika
中科院分区：
文献类型：
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作者：
S. Fabrika
（删节）该评论描述了 SS433 的观察结果。 SS433 和其他 X 射线双星之间的主要区别在于气体吸积到相对论性恒星（很可能是黑洞）的超临界状态，这导致了准直相对论性喷流的形成。射流的特性由它们与盘风的相互作用决定。圆盘和喷流的进动，以及双星系统中的食，使 SS433 成为研究微类星体现象机制的独特实验室。基本上，SS433 的所有光度和光谱特性均由吸积盘及其方向决定，但吸积盘本身位于浓密风的光球层下方，因此无法被观察到。描述了系统中风和气流的观测表现。人们对喷流热底座所在的中心区域的结构知之甚少。可用的 X 射线、紫外线和光学观测结果表明，喷流的底部被从喷流通道内部区域再辐射的热气体茧包围。直接研究 SS433 超临界吸积盘中的这个通道是不可能的；然而，类似的面向物体的正面可能是极其明亮的X射线源，例如在其他星系中观察到的超亮X射线源。
(abridged) The review describes observations of SS433. The main difference between SS433 and other X-ray binaries is the supercritical regime for the gas accretion onto the relativistic star (most likely a black hole), which has lead to the formation of collimated relativistic jets. The properties of the jets are determined by their interaction with the disk wind. The precession of the disk and jets, as well as the eclipsing in the binary system, make SS433 a unique laboratory for studies of mechanisms for the microquasar phenomenon. Essentially all photometric and spectroscopic properties of SS433 are determined by the accretion disk and its orientation, but the disk itself is not observed, being located beneath the photosphere of the dense wind. Observational manifestations of the wind and of gas flows in the system are described. Little is known about the structure of the central regions where the hot bases of the jets are located. The available X-ray, UV, and optical observations point towards the picture where the bases of the jets are surrounded by cocoons of hot gas reradiating emission from the inner regions of the jet channel. Direct investigations of this channel in the supercritical accretion disk of SS433 are not possible; however, a similar object oriented face-on would likely be an extremely bright X-ray source, such as ultra-luminous X-ray sources observed in other galaxies.