Analysis on the velocity field of non-spherical expansion of Planetary Nebulae

行星状星云（PNe）是由中等质量星星在其演化的渐近巨星分支阶段的物质抛射形成的。PNE由中心高温星星和电离气体组成。与HST获得的图像显示更复杂的气体流动比以前观察到的结果。本程序的目的是分析它们对应于HST图像的速度场，并解决在热中心星星辐射场作用下气体分布形状的问题。研究了在光学区域内保持空间信息的高色散光谱学，进而分析位置-速度图的方法。我们得到了如下结果：1.在<exp>PN G4-1晕中，在135° ~ 180°位置角方向上发现了速度为2 V_（=400- 600）km/s的类双极气流.在选定的PNe中还发现了大于2 V <exp>= 100 km/sec的高速气流。虽然样本PNe被限制在一个很小的数字，但它的频率似乎是50%。我们建立了观测模式，在几公里/秒的精度范围内分析PNe的速度场在不同的位置角。得到了IC 2149和NGC 6572的位置-速度图数据，认为PNe的各种形状是由于渐近巨分支阶段的星风与随后的非球形快速物质抛射相互作用的结果。为了应用发射线剖面分析方法，我们对共生星星; Z和在最近的爆发阶段进行了研究。我们的初步结果表明，由热矮星星星吸积引起的质量损失现象应该是造成宽翼分量的原因，其范围从几百到一千公里/秒。

Planetary Nebulae(PNe) are formed by mass ejection from intermediate mass star at the asymptotic giant branch phase in their evolution. PNe consist of the central high temperature star and the ionized gas. Images obtained with HST reveal much more complicated gaseous flows than previously observed results. Subject of this program is to analyze their velocity fields corresponding to images of HST, and to solve the problem how was the shape of gaseous distribution made under the radiation field of hot central star. Methods for researching this subject s high dispersion spectroscopy in optical regions keeping with spatial information and subsequently to analyze position-velocity diagram. We obtained following results.1. Bipolar like gas flow with large velocity 2V_<exp>=400-600km/sec was found in a halo PN G4-1 in the direction of position angle between 135°and 180°.2. We also found higher velocity gas flows than 2V_<exp>=100km/sec in selected PNe. Its frequency seems to be 50% although sample PNe are limited to a small number.3. We establish observational mode to analyze velocity fields of PNe within accuracy of a few km/sec in the various position angles. Data of position-velocity diagram have been obtained for IC 2149 and NGC 6572.In conclusion, it is considered that various shapes of PNe were made due to the interaction between stellar wind at the stage of asymptotic giant branch and subsequent non-spherical fast mass ejection. For the purpose of applying the method of emission-line profile analysis, we studied about symbiotic star; Z And during recent outburst phase. Our preliminary result suggests that mass losing phenomenon caused by accretion to hot dwarf star should be responsible to make a broad wing component ranging from several hundreds to one thousand km/sec.