位於大麥哲倫星雲當中超新星殘骸內的高速移動恆星

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姓名	陳鎮鴻(Chen-Hung Chen) 查詢紙本館藏	畢業系所	天文研究所
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 (Runaway stars in the supernova remnants in the Large Magellanic Cloud)
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摘要(中)	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。
摘要(英)	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.
關鍵字(中)	★ 天文 ★ 超新星殘骸 ★ 高速移動恆星	關鍵字(英)	★ Astronomy ★ Supernova remnant ★ Runaway stars
論文目次	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
參考文獻	[1] Baggett, S., McMaster, M., Biretta, J., et al. 2002, WFPC2 Instrument Handbook, Version 4.0 [2] Cantat-Gaudin, T., Jordi, C., Vallenari, A., et al. 2018, A&A, 618, A93 [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
指導教授	饒兆聰朱有花(Chow-Choong Ngeow You-Hua Chu)	審核日期	2019-8-24
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