研究領域 > 恆星形成
恆星形成
研究成果藝廊
請點選圖示瀏覽圖片解說
Dust distribution in the binary protostellar system L1551 NE observed with the SMA in 0.9 mm continuum.
恆星由分子雲形成,為宇宙最基本的組成份子。恆星形成的過程改變了分子雲的物理及化學環境,因此不僅控制了星系的結構和演化,也掌控了重元素逐步生成,及讓生命得以產生的行星環境。在如此的動力過程中,分子雲收縮產生了分子雲核,進而因重力坍縮形成年輕星體,接下來經由拱星盤發生物質吸積,這又伴隨著如恆星風,噴流或外向流導致物質流失,最終分子雲包層潰散。這只是我們所了解恆星形成的約略過程,但其細節尙未完全了解,故仍為現代天文學中的主要研究課題。本所恆星形成研究小組致力於以理論模型及觀測上的證據來了解恆形形成過程的本質。
研究人員 (24)
期刊論文 (471)
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- Phan-Bao N; Lee C-F; Ho PTP; Martin EL, "Submillimeter Array observations of the proto brown dwarf candidate SSTB213 J041757" , A&A: 564, A32, April, 2014 [SCI] ( ADS | Fulltext )
- Rao R; Girart JM; Lai SP; Marrone DP, "Detection of a Magnetized Disk around a Very Young Protostar" , ApJL: 780(1), L6, Jan, 2014 [SCI] ( ADS | Fulltext )
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- Hirashita H; Li Z-Y, "Condition for the formation of micron-sized dust grains in dense molecular cloud cores" , MNRAS: 434(1), L70-L74, July, 2013 [SCI] ( ADS | Fulltext )
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