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

行星状星云非球形膨胀速度场分析

• 批准号: 12640228
• 负责人: TAMURA Shinichi
• 金额: $ 1.6万
• 依托单位: Tohoku University
• 依托单位国家: 日本
• 项目类别: Grant-in-Aid for Scientific Research (C)
• 财政年份: 2000
• 资助国家: 日本
• 起止时间: 2000 至 2002
• 项目状态: 已结题
• 来源: https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-12640228/
• 关键词: Planetary Nebulae; Expanding Motion; Gaseous Shell Formation; Spectroscopic Observation; Emission Line

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.

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>晕PN G4-1中，在135° ~ 180°位置角方向上发现了类似双极的大速度气流2 V_ =400- 600 km/秒。2.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。

项目成果

S.Tamura: "High Velocity Flow Suggested by Wing Components of the Hα Line Profiles in the Selected Planetary Nebulae"Proc. IAU Symp. No.209 Planetary Nebulae : Their Evolution and Role in the Universe,2001. (in press).

S. Tamura：“选定行星状星云中 Hα 线轮廓的翼成分所暗示的高速流”Proc. IAU Symp. No.209 行星状星云：它们在宇宙中的演化和作用，2001 年。

M.Otsuka: "Analysis of Internal Motions in the Halo Planetary Nebula H4-1"Publ. Astr. Soc. Pacific. 115・1. 67-79 (2003)

M.Otsuka：“晕行星状星云 H4-1 的内部运动分析”Astr. 115・1。

Y.Ikeda: "Spectroscopic Diagnoses on Symbiotic Stars.III.Radial Velocity Analyses of HBV 475"Publ.Astr.Soc.Japan. 52・4. 589-599 (2000)

Y.Ikeda：“共生星的光谱诊断。III.HBV 475 的径向速度分析”Publ.Astr.Soc.Japan 52・4（2000）。

M.Otsuka: "Analysis on Internal Motions of the Halo Planetary Nebula, H4-1"Proc. IAU Symp. No.209 Planetary Nebulae : Their Evolution and Role in the Universe. (in press). (2003)

M.Otsuka：“晕行星状星云内部运动分析，H4-1”Proc。

S.Tamura: "Spectroscopic Diagnosis on Symbiotic Star Z And during Recent Outburst Phase"Proc. Pacific Rim Conference on Stellar Astrophysics. (in press). (2003)

S.Tamura：“共生星 Z 和最近爆发阶段的光谱诊断”Proc。