基于辐射水动力模拟的电离平衡计算的活动星系核统一模型
Unification Model of Active Galactic Nuclei by Photoionization Equilibrium Calculation Based on Radiative Hydrodynamic Simulations
AI总结：
本文通过辐射水动力模拟和电离平衡计算，研究了活动星系核覆盖因子与埃德蒙顿比的关系，并验证了计算结果与X射线观测的一致性。
摘要：
为了研究X射线观测所建议的覆盖因子与埃德蒙顿比依赖关系的起源，我们基于二维辐射水动力模拟研究了HI和HII的角分布。为了计算仅HI的Compton薄覆盖因子C22和Compton厚覆盖因子C24，我们基于辐射水动力模拟使用XSTAR代码进行了单维电离平衡计算。结果如下。(1) HI和HII的Compton薄覆盖因子C22与埃德蒙顿比无关，约为70%，而仅HI的C22也与埃德蒙顿比无关，约为30%。(2) HI的Compton厚覆盖因子C24的值与HI的C22相同。(3) 我们的C24与X射线观测所得结果一致。(4) 我们的C22在高埃德蒙顿比时与X射线观测结果一致，而在低埃德蒙顿比时比X射线观测结果小。(5) 为了解释理论计算所得C22与X射线观测所得C22之间的差异，需要在当前计算区域外至少延伸10 pc的Compton薄气体。
英文摘要：
To investigate the origin of the dependence of the covering factor on the Eddington ratio suggested by X-ray observations, we examined the angular distribution of HI and HII based on two-dimensional radiative hydrodynamic simulations. To calculate the Compton-thin covering factor $C_{22}$ and Compton-thick covering factor $C_{24}$ of HI alone, we performed one-dimensional photoionization equilibrium calculations with the XSTAR code based on radiative hydrodynamic simulations. The results obtained are as follows. (1) The Compton-thin covering factor $C_{22}$ of HI and HII is independent of the Eddington ratio and is approximately $70\%$, while $C_{22}$ of HI alone is also independent of the Eddington ratio and is approximately $30\%$. (2) The Compton-thick covering factor $C_{24}$ of HI has the same value as $C_{22}$ of HI. (3) Our $C_{24}$ is consistent with that obtained from X-ray observations. (4) Our $C_{22}$ agrees with that obtained from X-ray observations in a high Eddington ratio, while our $C_{22}$ is smaller than that from X-ray observations in a low Eddington ratio. (5) To explain the difference between $C_{22}$ obtained from theoretical calculations and that inferred from X-ray observations, a Compton-thin gas is required in regions extending at least $10~\mathrm{pc}$ beyond the current computational regions.
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