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研究生:陳鎮鴻
研究生(外文):Chen-Hung Chen
論文名稱:位於大麥哲倫星雲當中超新星殘骸內的高速移動恆星
論文名稱(外文):Runaway stars in the supernova remnants in the Large Magellanic Cloud
指導教授:饒兆聰朱有花
指導教授(外文):Chow-Choong NgeowYou-Hua Chu
學位類別:碩士
校院名稱:國立中央大學
系所名稱:天文研究所
學門:自然科學學門
學類:天文及太空科學學類
論文出版年:2019
畢業學年度:107
語文別:中文
論文頁數:45
中文關鍵詞:天文超新星殘骸高速移動恆星
外文關鍵詞:AstronomySupernova remnantRunaway stars
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在這篇論文當中,我們研究了大麥哲倫星雲中,位於超新星殘骸當中的高速移動 恆星。這些殘骸分別是 N63A,N9 與超級氣泡 N160。首先位於 N160 中,恆星的長縫 光譜表示了一顆高速恆星,並且在它的周遭環境發現了類似弓形震波的結構。假設個 系統達到衝壓力平衡,那根據它 Hα 的表面亮度與 [S II] λ6716/λ6731 的比值,我們可 以知道這個恆星的質量損失率應該小於 1.1 ± 0.5 × 10−5M⊙/yr.
而接著我們使用 Gaia DR2 的資料來研究兩個超新星殘骸 N9 與 N63A 中恆星的自 行速度。高速移動的恆星有可能以前是超新星的伴星,因此藉由研究自行速度能夠提 供我們一些可能以前是伴星的高速移動的恆星。在超新星殘骸 N9 中,有一顆看似跑得 很快的恆星。然而,它的周遭環境過於複雜導致我們需要更充足的觀測資料去更仔細 的了解它。而在超新星殘骸 N63A 當中,一個食雙星系統展露了高速的自行運動。然 而,在未來我們一樣需要更多的觀測資料去更仔細的了解這個系統。而研究的過程當 中,我們發現了一些有問題的高速自行運的的恆星。這些恆星大多其實是未被解析的 光學雙星或多星,導致他們的自行運動的速度分析很有可能是有問題的。因此,這提 醒我們檢查高解析影像的重要性。總結,我們這篇論文發現了三個可能是超新星伴星 的恆星或恆星系統。
We study runaway stars in the superbubble N160, supernova remnants (SNRs) N9 and N63A in the Large Magellanic Cloud (LMC). A runaway star in the superbubble N160 was diagnosed from its long-slit spectrum. A bow-shock-like structure was observed near this runaway. Assuming ram pressure equilibrium, the Hα surface brightness and the [S II] λ6716/λ6731 ratio gave the mass-loss rate not larger than 1.1±0.5×10−5M⊙/yr.
Gaia DR2 data were used to examine proper motions of massive stars in SNRs N9 and N63A to search for runaway stars as candidates for companions of their supernova progenitors. There is one star in N9 whose proper motion is large considered as the runaway star. However, the environment is so complex that it needs better observational data to confirm its natures. In the case of N63A, an eclipsing binary showed high proper motion. More observations and models are needed to explain the high proper motions of this binary and whether they are runaway companions or not in the future. We also noticed that some stars with large proper motion are actually unresolved multiple stars. The large proper motions of these stars are most likely spurious. Therefore, we note the importance of checking high-resolution images In summary, we diagnosed three runaway stars/binary that could be candidates for companions of SN progenitors in the LMC.
摘要................................................................... v
Abstract................................................................... vii
Contents................................................................... ix
List of Figures................................................................... xi
List of Tables................................................................... xiii
1 Introduction................................................................... 1
2 Diagnosing a runaway star in the superbubble N160 3
2.1 Discovery...................................................................... 3
2.2 Observation ................................................................... 4
2.3 Photometry.................................................................... 5
2.4 Radial velocity ................................................................ 6
2.5 Estimating the mass-loss rate.............................................. 10
3 Runaway stars in GAIA Data Release 2 15
3.1 Introduce GAIA............................................................... 15
3.2 Data analyses ................................................................. 15
3.3 SNR N9 ....................................................................... 16
3.4 SNR N63A .................................................................... 24
4 Conclusion.................................................................... 29
Bibliography .................................................................... 31
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[3] Chu, Y.-H. 1997, AJ, 113, 1815
[4] Erkal, D., Li, T. S., Koposov, S. E., et al. 2018, MNRAS, 481, 3148
[5] Gruendl, R. A., & Chu, Y.-H. 2009, ApJS, 184, 172
[6] Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2018, A&A, 616, A1
[7] Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1
[8] Lucke, R B. 1972, Ph.D. thesis, University of Washington
[9] Luri, X., Brown, A. G. A., Sarro, L. M., et al. 2018, A&A, 616, A9
[10] Maggi, P., Haberl, F., Kavanagh, P. J., et al. 2016, A&A, 585, A162
[11] Meixner, M., Gordon, K. D., Indebetouw, R., et al. 2006, AJ, 132, 2268
[12] Seward, F. D., Williams, R. M., Chu, Y.-H., et al. 2006, ApJ, 640, 327
[13] Smith, R. C., Chu, Y.-H., Mac Low, M.-M., Oey, M. S., & Klein, U. 1994, AJ, 108, 1266
[14] Shen, K. J., Boubert, D., Gänsicke, B. T., et al. 2018, ApJ, 865, 15
[15] Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163
[16] Vasiliev, E. 2018, MNRAS, 481, L100
[17] Whitney, B. A., Sewilo, M., Indebetouw, R., et al. 2008, AJ, 136, 18
[18] Zaritsky, D., Harris, J., Thompson, I. B., & Grebel, E. K. 2004, AJ, 128, 1606
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