论文标题
NGC 6153：现实很复杂
NGC 6153: Reality is complicated
论文作者
论文摘要
我们研究了基于NGC 6153中许多物理过程的发射线运动学，该运动线基于ESO VLT的uves光谱仪获得的深，空间分辨，高分辨率光谱。我们最基本的发现是NGC 6153中的血浆很复杂，尤其是其温度结构。大多数发射线的运动学定义了经典的扩展定律，外部膨胀最快（正常的肾上腺等离子体）。但是，\ ion {o} {1}的允许行，\ ion {c} {2}，\ ion {n} {2}，\ ion {o} {2}，\ ion {2}，\ ion {ne} {2} {2} {2} {2}呈现不断扩展的plas，以呈现一个恒定的knement knemem andemations commounts commounts commoundate andem commoundate（）。物理条件暗示了两个血浆成分，附加的血浆成分具有较低的温度和较高的密度。 [\ ion {o} {2}]密度和[\ ion {n} {2}]温度是异常的，但是考虑到重组对这些禁止线的贡献，可以理解。这两个等离子体成分的温度非常不同。正常的肾上腺血浆似乎在其体积的一部分（主壳）中有温度波动，但在其他地方只有很小的波动。额外的等离子体组件包含N $^{2+} $和O $^{2+} $ ions的一半，但仅$ 3-5 $ \％的h $^+$ ions的质量，因此两个质量成分具有非常不同的化学物质。我们估计$ 12+\ log（\ Mathrm O^{2+}/\ Mathrm H^+）\ SIM 9.2 $ \，DEX和$ \ MATHRM {HE}/\ MATHRM H \ SIM 0.13 $。尽管它们都是并发症，但多个等离子体成分，温度波动以及多个物理过程对给定发射线的贡献都是NGC 6153的现实的一部分，通常应考虑到。
We study the kinematics of emission lines that arise from many physical processes in NGC 6153 based upon deep, spatially-resolved, high resolution spectra acquired with the UVES spectrograph at the ESO VLT. Our most basic finding is that the plasma in NGC 6153 is complex, especially its temperature structure. The kinematics of most emission lines defines a classic expansion law, with the outer part expanding fastest (normal nebular plasma). However, the permitted lines of \ion{O}{1}, \ion{C}{2}, \ion{N}{2}, \ion{O}{2}, and \ion{Ne}{2} present a constant expansion velocity that defines a second kinematic component (additional plasma component). The physical conditions imply two plasma components, with the additional plasma component having lower temperature and higher density. The [\ion{O}{2}] density and the [\ion{N}{2}] temperature are anomalous, but may be understood considering the contribution of recombination to these forbidden lines. The two plasma components have very different temperatures. The normal nebular plasma appears to be have temperature fluctuations in part of its volume (main shell), but only small fluctuations elsewhere. The additional plasma component contains about half of the mass of the N$^{2+}$ and O$^{2+}$ ions, but only $3-5$\% of the mass of H$^+$ ions, so the two plasma components have very different chemical abundances. We estimate abundances of $12+\log(\mathrm O^{2+}/\mathrm H^+)\sim 9.2$\,dex and $\mathrm{He}/\mathrm H\sim 0.13$. Although they are all complications, multiple plasma components, temperature fluctuations, and the contributions of multiple physical processes to a given emission line are all part of the reality in NGC 6153, and should generally be taken into account.
