吸积率

在本文中我们通过AGB星研究了此临界吸积率和金属丰度之间的关系。

In this thesis , we study the relation between the critical accretion rate and the metallicity via AGB stars approach .

当描述磁场的参数λ越大的时候，磁化EWCS的吸积率越大。

When the parameter X is larger , the core accretion rate appropriate for magnetized EWCS is larger .

当吸积率小于临界吸积率时，盘结构有唯一的稳态解，大于临界吸积率则没有稳态解。

There is one solution for disk structure if the rate is lower the the critical rate .

然而，物理上合理的整体解却是唯一的，它总是使两个吸积率值中之较小者得到实现。

However , the physically acceptable global solution is unique : it is always realized for the smaller of the two accretion rates .

通过模拟分析得出，随着吸积率的变化，中心黑洞质量和热光度也在变化。

From these analyses , we found that the black hole masses and the luminosity of AGN_S change with the development of accretion rate .

结果表明，在吸积率一定的情况下，该功率主要决定于a，对ε′不敏感，且计算得到的功率能很好地拟合喷流功率的观测数据值。

The result shows that under certain condition of given accretion rate , the power mainly depends on α _ and insensitive to ε′ . The calculated powers can be used to properly match the observed data of jet powers .

在各种前身星模型中最流行的是单简并钱德拉塞卡质量极限模型，但此模型的吸积过程中存在一个临界吸积率问题。

The most favoured model among various progenitor models is the single degenerate Chandrasekhar mass model , but there exists a critical accretion rate for the progenitor system .

Bondi（1952年）研究了恒星对静态气体的吸积问题，确定了引力捕获半径和得到了Bondi吸积率。

In 1952 , Bondi solved the hydrodynamic version of the star in a static ambient medium , who showed a certain gravitational capture radius , got Bondi accretion rates .

Bondi吸积可称为高态而盘吸积为低态，因为前者总对应着较高的吸积率。

The Bondi type accretion defines a high state and the disk type a low state , in the sense that the former always requires a higher accretion rate .