星团在黑洞上的吸积。I.丛状-ADAF结构和辐射
Clumpy accretion onto black holes. I. Clumpy-ADAF structure and radiation
摘要：
在本文中，我们研究嵌入并限制在对流为主的吸积流（ADAF），其中忽略了碰撞的块动力学。我们从无碰撞玻尔兹曼方程出发，假设团簇和ADAF之间的相互作用负责向外传输团簇的角动量。块ADAF的内边缘被设置为块的潮汐半径。我们考虑了强耦合和弱耦合的情况，其中团块的平均性质遵循ADAF动力学，并主要由黑洞潜力，分别。得到了这两种情况下团簇动力学的解析解。在强耦合的情况下，团簇的速度色散比ADAF高一个数量级。对于弱耦合情况，我们发现团簇的平均径向速度与曳力系数成线性关系。我们表明，潮汐破坏团块将导致积累的碎片，形成碎片盘在Shakura-Sunyaev制度。整个热的ADAF将被来自碎片盘的光子有效地冷却下来，从而引起ADAF的坍缩并淬灭星团吸积。随后，塌陷的ADAF的蒸发驱动新的团簇ADAF的复苏，导致全球团簇ADAF的振荡。简要讨论了本模型在X射线双星、电离核发射区和BL Lac天体中的应用。
英文摘要：
In this paper, we investigate the dynamics of clumps embedded in and confined by the advection-dominated accretion flows (ADAF), in which collisions among the clumps are neglected. We start from the collisionless Boltzmann equation and assume that interaction between the clumps and the ADAF is responsible for transporting angular momentum of clumps outward. The inner edge of the clumpy-ADAF is set to be the tidal radius of the clumps. We consider strong and weak coupling cases, in which the averaged properties of clumps follow the ADAF dynamics and mainly determined by the black hole potential, respectively. We get the analytical solution of the dynamics of clumps for the two cases. The velocity dispersion of clumps is one magnitude higher than the ADAF for the strong coupling case. For the weak coupling case, we find that the mean radial velocity of clumps is linearly proportional to the coefficient of the drag force. We show that the tidally disrupted clumps would lead to accumulation of the debris to form a debris disk in the Shakura-Sunyaev regime. The entire hot ADAF will be efficiently cooled down by photons from the debris disk, giving rise to collapse of the ADAF and quench the clumpy accretion. Subsequently, evaporation of the collapsed ADAF drives resuscitate of a new clumpy-ADAF, resulting in an oscillation of the global clumpy-ADAF. Applications of the present model are briefly discussed to X-ray binaries, ionization nuclear emission regions (LINERs) and BL Lac objects.
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