博碩士論文 102229004 詳細資訊




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姓名 張瀚元(Chang, Han-Yuan)  查詢紙本館藏   畢業系所 天文研究所
論文名稱
(Flare activities of M dwarfs in the Kepler data archjw with LAMOST observation)
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摘要(中) M 型主序星通常是有著接近或完全對流的外層,由於他們對流的外層產生 強烈的磁場,常常可以在光譜上有見到色球層的 Hα 譜線的 M 型主序星也會有 閃焰的發生。另外,跟 G 型主序星(類似太陽的恆星)相比,M 型主序星的適 居帶非常靠近他們主星,對於在 M 型主序星適居帶上的系外行星的適居性可能 會受到閃焰的影響,因此研究 M 型主序星的閃焰一個有趣的研究題目。
本篇論文是用了 Kepler 太空望遠鏡的資料以及 LAMOST 望遠鏡的光譜資 料來做研究,主要的 M 型主序星都是屬於 M0 到 M3 的分類,從 Kepler 的觀測 資料中計算出來的自轉週期跟閃焰的大小、閃焰頻率分布的指數、以及 Hα 譜 線的等值寬度有密切的關聯,可以看到有明顯的趨勢在快速自轉(自轉週期低 於 15 天)的 M 型主序星上。
摘要(英) The M dwarfs are usually known with their convective envelopes. Due to the strong magnetic activities associated with their convective envelopes, M dwarfs showing strong chromospheric emission in Hα line have large flare activities in general. Moreover, comparing with G dwarfs, the habitable zone is much closer to M dwarfs. The habitability of the exoplanet might be affected by flares of M dwarfs and, therefore, it is interesting to investigate the flare phenomena of M dwarfs.
This thesis provides a sample of the LAMOST spectra of the early M dwarfs (i.e., M0 – M3) to compare with the Kepler observations. The rotational periods derived from the Kepler measurements are highly correlated with flare intensity, the power-law index of distribution and the equivalent widths of the Hα line emission. We found that fast rotating (i.e., rotational periods < 15 day) M dwarfs have more magnetic activities.
關鍵字(中) ★ 恆星
★ 恆星活動
★ 恆星閃焰
★ M型恆星
★ 低質量恆星
關鍵字(英) ★ stars
★ activity - stars
★ flare - stars
★ late-type - stars
★ low-mass - stars
論文目次 Contents
摘要 i
Abstract ii
致謝 iii
Contents iv
List of Figures v
List of Table vii
1. Introduction 1
1.1 Flares research by Kepler 2
1.2 M dwarf flares 2
1.3 LAMOST observation of M dwarfs in Kepler field 3 2. Kepler Mission 4
2.1 Kepler data acquiring and selection 5
2.2 Kepler data analysis 6
2.3 Detrending 10
2.4 Flare Detection 12
2.5 Flare energy 14
2.6 Flare frequency distribution 15
2.7 Rotation period 17
3. LAMOST 20
3.1 LAMOST telescope 20
3.2 LAMOST observation of M dwarfs 21
4. Result 24
4.1 Comparison with period 24
4.2 Comparison with Hα emission 27
5. Summary and Discussions 29
Bibliography 30
Appendix 31
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指導教授 葉永烜(Ip, Wing-Huen) 審核日期 2016-8-30
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