arXiv 0905.21482009-05-13astro-ph.SRastro-ph.IM

行星状星云NGC 7009的三维速度结构

The 3D velocity structure of the planetary nebula NGC 7009

W. Steffen, M. Espindola, S. Martinez, N. Koning

备注：: accepted for publication in Revista Mexicana de Astronomia y Astrofisica (RevMexAA), 13 pages, 11 figures; pdf file with full quality images can be retrieved from http://www.astrosen.unam.mx/shape

摘要：

为了寻找行星状星云同系膨胀的偏差，我们提出了一个NGC 7009的三维形态运动学模型。该模型已被构建与{ \em形状}的基础上，从文献和HST图像的PV图。我们发现，这些数据是一致的径向速度场增加梯度在高纬度地区相比，赤道地区（模型1）。在第二个模型中，我们假设在$70^\circ$附近的纬度上，径向速度分量线性增加，并增加了10 km/s量级的极向分量。真实的速度场很可能介于这两种极限情况之间。我们还发现，膨胀的袢是非径向的中央恒星。它们的速度场集中在主壳的视出口点附近。我们预测的适当运动模式的模型与非零极向速度分量。

英文摘要：

In search for deviations from homologous expansion in planetary nebulae we present a 3D morphokinematical model of NGC 7009. The model has been constructed with {\em Shape} based on PV diagrams from the literature and HST images. We find that the data are consistent with a radial velocity field with increased gradient at high latitudes compared to the equatorial region (Model 1). In a second model we assume a linearly increasing radial velocity component with an added poloidal component of order 10 km/s at latitudes around $70^\circ$. The true velocity field is likely to be in between these two limiting cases. We also find that the expansion of the ansae is non-radial with reference to the central star. Their velocity field is focused near the apparent exit points from the main shell. We predict the proper motion pattern for the model with a non-zero poloidal velocity component.

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