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    Please use this identifier to cite or link to this item: http://ir.lib.ncu.edu.tw/handle/987654321/6014

    Title: 行星狀星雲Hα結構之分析;Structures of the H-alpha halos of Planetary Nebulae from the SHASSA observations
    Authors: 夏志浩;Chih-Hao Hsia
    Contributors: 天文研究所
    Keywords: 交互作用恆星風模型;暗暈;行星狀星雲;Planetary Nebulae;Halos
    Date: 2003-06-27
    Issue Date: 2009-09-22 10:11:54 (UTC+8)
    Publisher: 國立中央大學圖書館
    Abstract: 行星狀星雲(Planetary Nebulae)乃是中、小質量恆星演化到末期的必然結果, 而其複雜的結構正好提供我們一個理想的天文物理實驗室; 尤其是近年來天文儀器的進步, 更是使得行星狀星雲的研究進展非常迅速。 郭新(Sun Kwok)在1978年提出交互作用恆星風模型, 當時他預測行星狀星雲將有較暗的光暈存在。但是目前在44個行星狀星雲中, 只有找到66% 的行星狀星雲有光暈的存在。 對於行星狀星雲而言, 光暈的存在正是意味著行星狀星雲的起源, 我們唯有藉著行星狀星雲的光暈才能夠了解行星狀星雲之前的演化過程。 由於行星狀星雲的光暈是紅巨星或是漸進巨星分支 時質量損失的過程, 我們分別利用南半天球的Hα 巡天觀測以及一米望遠鏡(LOT)針對光暈結構進行Hα 的窄波段觀測。 在這些觀測中, 我們藉著104個比以往還要大的行星狀星雲光暈結構, 成功的證實了交互作用恆星風模型的預測; 還找到了其中6個行星狀星雲正與星際介質進行交互作用以及它們所形成的特徵結構。 不僅僅如此, 我們利用測得光暈的流量來估計其質量的大小。 我們也發現光暈與行星狀星雲在形態上並沒有什麼相關性, 這與理論上的推測相當吻合。 在未來我們將會藉由其他高解析的望遠鏡對於這些與星際介質交互作用的行星狀星雲進行觀測, 以期獲得更多關於這些特徵結構的資料。 Planetary nebulae mark the endpoint of stellar evolution. The complex structures of Planetary Nebulae can offer a perfect astrophysical Lab. We think that better instruments make the study of Planetary Nebulae quickly. Prof.. Sun Kwok suggest Interactive Stellar Wind Model in 1978.He forecasted that there are faint halos surrounding Planetary Nebulae. People had studied 66% Planetary Nebulae were found to have extended halos. The meaning of halo is the origin of Planetary Nebulae. We can get more information about the evolution before Planetary Nebulae by the faint halos. We use the database of SHASSA and observe the structure of halo with LOT in Hα. In the observations, we had found the faint halo in 104 Planetary Nebulae and discover the characteristic structures interactive with Interstellar Medium(ISM) in 6 Planetary Nebulae. We find there is no correlate with the halos and the morphology of Planetary Nebulae. It is similar with the forecast of theory. Besides, we detected the mass of halos of Planetary Nebulae by the flux of images. We will get more time to observe the structures interactive with ISM by high-resolution telescopes
    Appears in Collections:[天文研究所] 博碩士論文

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