The Emission Line Regions of Active Nuclei and Classical Novae

将对暴露在电离辐射下的气体中的物理条件进行数值模拟。这一结果将应用于当前在理解活动星系核和新星光谱方面的几个问题。对名为“云”的光电离化代码的改进将主要在以下几类方面：a)原子数据库的改进将继续进行；b)物理过程的处理将继续得到加强和更加完善；c)线转移方法和假设将得到改进。这些对计算有效性的持续改进是重要的，因为“多云”已被广泛的用户用来研究各种物理情况：a)活动核的宽线区域，在那里将研究一种替代的气体排放模型；B)塞弗特星系NGC4151中扩展的X射线发射气体，该区域可能是康普顿热风的一个例子；c)旧新星DQ Hercules周围的星云，由于温度非常低(约500K)和中等电离水平而独特。理论和观测之间的这种对抗是电离气体数值模拟继续发展的重要组成部分。

Numerical simulation of the physical conditions in gas exposed to ionizing radiation will be carried out. The results will be applied to several current problems in understanding the spectra of active galactic nuclei and novae. The improvements to the photoionization code named "CLOUDY" will largely be in the following categories: a) the improvement in the atomic data base will be continued; b) the treatment of physical processes will continue to be enhanced and made more complete; and c) the line transfer methods and assumptions will be improved. These continued enhancements to the of validity of the calculations are important since "CLOUDY" has been employed by a wide community of users to study a variety of physical situations; a) the broad line region of active nuclei, where an alternative model of emitting gas will be investigated; b) the extended x-ray emitting gas in the Seyfert galaxy NGC 4151, a region which may be an example of Compton heated wind; and c) the nebula around the old nova DQ Hercules, unique because of the very low temperature (approximately 500k) and moderate level of ionization. Such confrontation between theory and observation is an important ingredient in the continued development of numerical simulations of ionized gas.