光学薄日冕超精细结构线的可观测性
On the Observability of Optically Thin Coronal Hyperfine Structure Lines
摘要：
我们提出了在各种环境下日冕超精细线强度的云计算。我们模拟间接碰撞和辐射跃迁，并在密度-温度相空间中量化碰撞激发线发射率。作为观测的辅助，我们还表示在0.4- 0.7千电子伏波段的连续辐射率的单位。对于大多数超精细线，X射线表面亮度和等离子体温度的知识是足够的粗略估计。我们发现，英仙座A和室女座A的辐射场可以提高人口的高度电离的物种在1千秒差距。它们还可以增强簇芯内的线发射率。这可能对解释明亮活动星系核周围的光谱有影响。我们发现$^{57}$ Fe XXIV λ3.068 mm的强度比以前认为的要弱两个数量级，大约在20 μK。在红外线中可以找到相当亮的线。最后，我们发现扩展猎户座星云中的超精细线的强度很低，这是由于视线较浅。利用下一代射电望远镜和亚毫米望远镜观测日冕超精细线可能是可行的。
英文摘要：
We present Cloudy calculations for the intensity of coronal hyperfine lines in various environments. We model indirect collisional and radiative transitions, and quantify the collisionally-excited line emissivity in the density-temperature phase-space. As an observational aid, we also express the emissivity in units of the continuum in the 0.4--0.7 keV band. For most hyperfine lines, knowledge of the X-ray surface brightness and the plasma temperature is sufficient for rough estimates. We find that the radiation fields of both Perseus A and Virgo A can enhance the populations of highly ionized species within 1 kpc. They can also enhance line emissivity within the cluster core. This could have implications for the interpretation of spectra around bright AGN. We find the intensity of the $^{57}$Fe XXIV λ3.068 mm to be about two orders of magnitude fainter than previously thought, at about 20 μK. Comparably bright lines may be found in the infrared. Finally, we find the intensity of hyperfine lines in the Extended Orion Nebula to be low, due to the shallow sightline. Observations of coronal hyperfine lines will likely be feasible with the next generation of radio and sub-mm telescopes.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
