局域气泡的非平衡电离模型（I）
A non-equilibrium ionization model of the Local Bubble (I)
摘要：
目标。本文首次对湍流超新星驱动的星际介质中局域泡和圈I超泡的联合演化进行了高分辨率非平衡电离模拟。详细研究了类锂离子Civ、Nv和Ovi在LB中的时间变化和空间分布。方法.这项工作使用并行自适应网格细化代码EAF-PAMR耦合到新开发的原子和分子等离子体发射模块E（A+M）PEC，具有通过Fe的H的电离结构的随时间变化的计算，使用最新的太阳丰度的修订。AMR最好的分辨率是在一个网格内的1 pc，该网格覆盖了银河系盘（中平面上的面积为1 kpc ^2）和晕（中平面上下延伸至10 kpc）的代表性补丁。结果LB的演化年龄是由模拟和观察到的类锂离子Civ，Nv和Ovi的吸收特性之间的匹配。模拟的LB电流演化时间在0.5到0.8百万年之间，因为最后一颗超新星重新加热了空腔，以便在模拟的LB空腔内使N（Ovi）< 8 \times 10^12 cm-2，log[N（Civ）/N（Ovi）] < -0.9和log[N（Nv）/N（Ovi）] < -1，正如哥白尼，IUE，GHRS-IST和FUSE观测所发现的那样。
英文摘要：
Aims. We present the first high-resolution non-equilibrium ionization simulation of the joint evolution of the Local Bubble (LB) and Loop I superbubbles in the turbulent supernova-driven interstellar medium (ISM). The time variation and spatial distribution of the Li-like ions Civ, Nv, and Ovi inside the LB are studied in detail. Methods. This work uses the parallel adaptive mesh refinement code EAF-PAMR coupled to the newly developed atomic and molecular plasma emission module E(A+M)PEC, featuring the time-dependent calculation of the ionization structure of H through Fe, using the latest revision of solar abundances. The finest AMR resolution is 1 pc within a grid that covers a representative patch of the Galactic disk (with an area of 1 kpc^2 in the midplane) and halo (extending up to 10 kpc above and below the midplane). Results. The evolution age of the LB is derived by the match between the simulated and observed absorption features of the Li-like ions Civ, Nv, and Ovi . The modeled LB current evolution time is bracketed between 0.5 and 0.8 Myr since the last supernova reheated the cavity in order to have N(Ovi) < 8 \times 10^12 cm-2, log[N(Civ) /N(Ovi) ] < -0.9 and log[N(Nv) /N(Ovi) ] < -1 inside the simulated LB cavity, as found in Copernicus, IUE, GHRS-IST and FUSE observations.
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