吸积盘整体结构的统一描述

A Unified Description of the Global Structure of Accretion Disks

在考虑径向对流和不同光学厚度的基础上，我们采用一般的辐射致冷假设；在统一的框架内考察了吸积盘的整体结构．对α模型，我们发现在不同的盘区存在不同的整体结构．在吸积率较低时，存在三种类型解：光学厚的局部辐射致冷解；光学薄的局部致冷解；光学薄的对流致冷解．这些解在盘内较大范围内都存在且互不交叉．但在吸积率较高和粘滞系数较大时，两种局部致冷解会相互交叉，而对流为主的解在所有盘区都稳定存在．另一方面，在吸积率较高和粘滞系数较小时，两种光学薄解会相互交叉，而光学厚和局部致冷为主的解在所有盘区都存在．

The global structure of accretion disks is investigated in a unified scheme by applying a general radiative cooling formula which can be used in both the optically thick and thin regimes and also including the radial advective heat transport. Within the framework of a-viscosity models, we find that there are distinctive families of global solutions exist in dtherent ranges of disk radii. For low mass accretion rate. M, there are three families which are: optically thick and local radiative cooling, optically thin and local cooling, and optically thin and advection cooling. These solutions extend a wide range of disk radii and do not cross with each other. However, for high M and large viscosity parameter, α, the two local cooling solutions cross with each other at radii R1 and R2. They form two families of solutions which ekist in regions R < R1 and R > R2 respectively. The gap between R1 and Ra increases as M increases, whereas the advection dominated solution ekists at all radii and is stable. For high M and small at on the other hand, the two optically thin solutions cross with each other at radii R3 and R4. The size of this region decreases as M increase; on the other hand, the optically thick and local cooling dominated solution ekists at all radii.