“距离映射”和BB的三维结构+30 3639
"Distance mapping" and the 3-D structure of BB +30 3639
摘要：
BD +30 3639是一组不常见的行星状星云的成员，它的中心恒星是沃尔夫-拉叶星，其[O III]线的膨胀速度比[N II]线的膨胀速度高。图像和高分辨率光谱从文献中使用，以构建一个3-D模型的星云使用形态运动学代码SHAPE。我们发现[N II]和[O III]壳层需要两个同系膨胀律。我们得出结论，BD +30 3639的内部速度场至少在[O III]和[N II]壳层之间随着与中心恒星的距离而减小。一个圆柱形的速度组件被用来复制高速双极准直流出。我们还提出了一种新的运动分析技术称为“距离映射”。它使用所观察到的适当的运动矢量和3-D速度场生成的地图，可以作为一个约束的形态运动学建模与SHAPE，以及提高距离确定的准确性。利用Li等人（2002）的178个内部自行矢量和我们的三维速度场将其应用于BD+30 3639，以确定1.52 \pm 0.21 kpc的距离。最后，我们发现了星云东部与周围H2分子气体相互作用的证据。
英文摘要：
BD +30 3639 is a member of a group of uncommon planetary nebula with Wolf-Rayet central star and higher expansion velocities in [O III] than in [N II] lines. Images and high-resolution spectra from the literature are used in order to construct a 3-D model of the nebula using the morpho-kinematic code SHAPE. We find that two homologous expansion laws are needed for the [N II] and [O III] shell. We conclude that the internal velocity field of BD +30 3639 decreases with the distance from the central star at least between the [O III] and [N II] shells. A cylindrical velocity component is used to replicate the high-speed bipolar collimated outflows. We also present a new kinematic analysis technique called "distance mapping". It uses the observed proper motion vectors and the 3-D velocity field to generate maps that can be used as a constraint to the morpho-kinematic modeling with SHAPE as well as improve the accuracy for distance determination. It is applied to BD+30 3639 using 178 internal proper motion vectors from Li et al. (2002) and our 3-D velocity field to determine a distance of 1.52 \pm 0.21 kpc. Finally, we find evidence for an interaction between the eastern part of nebula and the ambient H2 molecular gas.
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