论文标题
高密度行星星云中的丰度差异因子
Abundance Discrepancy Factors in high density planetary nebulae
论文作者
论文摘要
从高分辨率光谱中，已经确定了碰撞激发线（CELS）和光学重组线（ORL）的化学丰度（ORL）对于行星星云CN 3-1，VY 2-2，HU 2-1，HU 2-1，VY 1-2，VY 1-2和IC 4997，它们是年轻和密度的物体。这项工作的主要目的是推导其o $^{+2} $/h $^{+} $丰度差异因子，ADF，CELS和ORL之间。获得了他，O，N，NE，AR，S和CL丰度，我们的价值与先前报告的值一致。我们发现CN 3-1，HU 2-1和VY 1-2具有典型的圆盘pne的丰度，而VY 2-2和IC 4997是低O的物体（$ \ rm {12+log（o/h）\ sim 8.2} $），这可以归因于depletion deppletion中的粉尘颗粒。 $ 4.30^{+1.00} _ { - 1.16} $，$ 1.85 \ pm 1.05 $，$ 5.34^{+1.27} _ { - 1.27} _ { - 1.08} $和$ 4.87^$ 4.87^{+4.34} $ vy vy for vy， IC 4997。为每种情况分析了CELS和ORL的运动学，以研究星云中不同的等离子体发出的可能性。 [O III]和O II的膨胀速度在三个PNE的不确定性中是平等的，没有证据表明这些线在不同区域中排放。 HU 2-1和VY 2-2例外，其中ORL可能在不同的区域中发出的区域与CELS不同。对于VY 2-2和IC 4997，我们发现相同离子的Nebular和Auroral线（S $^+$，N $^{+} $，ar $^{+2} $，ar $^{+3} $，O $^{+2} $）可能会带来不同的扩张速度。极光线显示较低的$ \ rm {v_ {exp}} $，这可能表明它们在较密集的区域和内部区域中发射。
From high-resolution spectra, chemical abundances from collisionally excited lines (CELs) and optical recombination lines (ORLs) have been determined for planetary nebulae Cn 3-1, Vy 2-2, Hu 2-1, Vy 1-2 and IC 4997, which are young and dense objects. The main aim of this work is to derive their O$^{+2}$/H$^{+}$ Abundance Discrepancy Factors, ADFs, between CELs and ORLs. He, O, N, Ne, Ar, S, and Cl abundances were obtained and our values are in agreement with those previously reported. We found that Cn 3-1, Hu 2-1, and Vy 1-2 have O abundances typical of disc PNe, while Vy 2-2 and IC 4997 are low O abundance objects ($\rm{12+log(O/H) \sim 8.2}$), which can be attributed to possible O depletion into dust grains. ADFs(O$^{+2}$) of $4.30^{+1.00}_{-1.16}$, $1.85 \pm 1.05$, $5.34^{+1.27}_{-1.08}$ and $4.87^{+4.34}_{-2.71}$ were determined for Vy 2-2, Hu 2-1, Vy 1-2 and IC 4997, respectively. The kinematics of CELs and ORLs was analysed for each case to study the possibility that different coexisting plasmas in the nebula emit them. Expansion velocities of [O III] and O II are equal within uncertainties in three PNe, providing no evidence for these lines being emitted in different zones. Exception are Hu 2-1 and Vy 2-2, where ORLs might be emitted in different zones than CELs. For Vy 2-2 and IC 4997 we found that nebular and auroral lines of the same ion (S$^+$, N$^{+}$, Ar$^{+2}$, Ar$^{+3}$, O$^{+2}$) might present different expansion velocities. Auroral lines show lower $\rm{V_{exp}}$ which might indicate that they are emitted in a denser and inner zone than the nebular ones.
