Infrared coronal emission lines and the possibility of their laser emission in Seyfert nuclei
Infrared coronal emission lines and the possibility of their laser emission in Seyfert nuclei
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红外日冕发射线及其在赛弗特核中激光发射的可能性
DOI：
10.1086/191813
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发表时间：
1993
影响因子：
8.7
通讯作者：
A. Bar
中科院分区：
文献类型：
--
作者：
M. Greenhouse;U. Feldman;H. Smith;M. Klapisch;A. Bhatia;A. Bar
高能发射区传统上是通过X射线，紫外线和光学发射线的高度电离的中等质量的元素。这种线通常被称为“日冕线”，因为离子，当由碰撞电离产生时，在电子温度约为100 ℃时达到最大丰度。10（exp 5）- 10（exp 6）K典型的太阳上层大气。然而，光学和紫外日冕线也在各种各样的银河系和河外源，包括银河系星际介质，新星壳，超新星遗迹，星系和类星体中观察到。红外日冕线提供了一个新的窗口，观测高能发射区在严重的尘埃遮蔽的来源，如红外明亮的合并星系和塞弗特核和新的机会，模型的限制，在这些来源的物理条件。与它们的紫外和光学对应物不同，红外日冕线可以是碰撞电离等离子体的主要冷却剂，其10（exp 4）小于T（sub e）（K）小于10（exp 6），其产生很少或没有光学或更短波长的日冕线发射。此外，它们还提供了一种手段来探测灰尘严重遮蔽的发射区域，这些区域通常无法进行光学或紫外线研究。在这张海报中，我们提供了新模型计算的结果，以支持即将到来的红外空间天文台（ISO）和目前的地面观测计划，涉及AGN中的红外日冕发射线。我们提供了一个完整的红外列表（λ大于1微米）线，这是由于接地配置2s（2）2 p（k）和3s（2）3 p（k）内的过渡（k = 1 ~ 5）或高电离态的第一激发组态2s 2 p和3s 3 p（x大于或等于100 eV）天体物理丰富（n（X）/n（H）大于或等于10（exp-6））元素。包括O、Ne、Na、Mg、Al、Si、S、Ar、Ca、Fe和Ni的离子的大约74条谱线，其跨越大约1 - 280微米的波长范围。我们提出了新的结果，从详细的平衡计算，新的临界密度碰撞去激发，固有的光子速率，分支比，和激发温度的大多数编译转换。给出了红外日冕线主导冷却的温度和密度参数空间，讨论了红外日冕线与光学日冕线的关系。
Energetic emitting regions have traditionally been studied via x-ray, UV and optical emission lines of highly ionized intermediate mass elements. Such lines are often referred to as 'coronal lines' since the ions, when produced by collisional ionization, reach maximum abundance at electron temperatures of approx. 10(exp 5) - 10(exp 6) K typical of the sun's upper atmosphere. However, optical and UV coronal lines are also observed in a wide variety of Galactic and extragalactic sources including the Galactic interstellar medium, nova shells, supernova remnants, galaxies and QSOs. Infrared coronal lines are providing a new window for observation of energetic emitting regions in heavily dust obscured sources such as infrared bright merging galaxies and Seyfert nuclei and new opportunities for model constraints on physical conditions in these sources. Unlike their UV and optical counterparts, infrared coronal lines can be primary coolants of collisionally ionized plasmas with 10(exp 4) less than T(sub e)(K) less than 10(exp 6) which produce little or no optical or shorter wavelength coronal line emission. In addition, they provide a means to probe heavily dust obscured emitting regions which are often inaccessible to optical or UV line studies. In this poster, we provide results from new model calculations to support upcoming Infrared Space Observatory (ISO) and current ground-based observing programs involving infrared coronal emission lines in AGN. We present a complete list of infrared (lambda greater than 1 micron) lines due to transitions within the ground configurations 2s(2)2p(k) and 3s(2)3p(k) (k = 1 to 5) or the first excited configurations 2s2p and 3s3p of highly ionized (x greater than or equal to 100 eV) astrophysically abundant (n(X)/n(H) greater than or equal to 10(exp -6)) elements. Included are approximately 74 lines in ions of O, Ne, Na, Mg, Al, Si, S, Ar, Ca, Fe, and Ni spanning a wavelength range of approximately 1 - 280 microns. We present new results from detailed balance calculations, new critical densities for collisional de-excitation, intrinsic photon rates, branching ratios, and excitation temperatures for the majority of the compiled transitions. The temperature and density parameter space for dominant cooling via infrared coronal lines is presented, and the relationship of infrared to optical coronal lines is discussed.