无耗散椎间盘的积聚和血浆流出
Accretion and plasma outflow from dissipationless discs
摘要：
我们考虑一个极端的情况下，光盘吸积到一个引力中心时，在光盘的粘度可以忽略不计。吸积物质的角动量和转动能是由从圆盘流出的磁化风携带的。物质从圆盘中流出是由于Blandford & Payne（1982）的离心机制。假设圆盘是冷的。吸积和流出由能量守恒、质量守恒和角动量守恒联系起来。外流的基本性质，角动量通量和能量通量的每个粒子在风中，不依赖于吸积盘的结构的细节。在自相似吸积/流出的情况下，吸积率$\dot M$在光盘依赖于光盘半径$r$的法律$\dot M \sim r^{1\over2(α^2-1)}$，其中$α$是一个无量纲阿尔文半径。在$α\gg 1$的情况下，盘中的吸积是由盘中非常弱的物质流出提供的，并且流出主要发生在盘的非常中心的部分。在工作中获得的解决方案提供的机制，转换成外流风的能量的效率接近100%的吸积物质的引力能。最终的速度可以基本上超过开普勒速度在风发射的网站。这种机制使我们能够理解具有低光度盘和高能喷流的天体物理对象的性质。
英文摘要：
We consider an extreme case of disc accretion onto a gravitating centre when the viscosity in the disc is negligible. The angular momentum and the rotational energy of the accreted matter is carried out by a magnetized wind outflowing from the disc. The outflow of matter from the disc occurs due to the Blandford & Payne(1982) centrifugal mechanism. The disc is assumed to be cold. Accretion and outflow are connected by the conservation of the energy, mass and the angular momentum. The basic properties of the outflow, angular momentum flux and energy flux per particle in the wind, do not depend on the details of the structure of the accretion disc. In the case of selfsimilar accretion/outflow, the dependence of the rate of accretion $\dot M$ in the disc depends on the disc radius $r$ on the law $\dot M \sim r^{1\over2(α^2-1)}$, where $α$ is a dimensionless Alfvenic radius. In the case of $α\gg 1$, the accretion in the disc is provided by very weak matter outflow from the disc and the outflow predominantly occurs from the very central part of the disc. The solution obtained in the work provides mechanism which transforms the gravitational energy of the accreted matter into the energy of the outflowing wind with efficiency close to 100%. The final velocity can essentially exceed Kepler velocity at the site of the wind launch. This mechanism allows us to understand the nature of the astrophysical objects with low luminosity discs and energetic jet-like outflows.
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