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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)相關論文 檔案 [Endnote RIS 格式]
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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 31參考文獻 Balona L. A., 2012, MNRAS, 423, 3420
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