Description: 原恆星是恆星形成過程的早期階段。它是星際介質中巨大分子雲收縮後形成的大量氣體和塵埃。隨著分子雲的坍縮，引力勢能轉化為熱能，使仍在形成中的原恆星升溫。這一階段可能需要 10⁵ 到 10⁷ 年，具體時間取決於恆星的質量，質量越大的恆星形成得越快。這個過程始於分子雲核心密度的增加，終於前主序星的形成。質量與太陽相近的前主序星被稱為金牛座T型恆星（T-Tauri）。一旦恆星內的氫聚變被點燃，它就開始產生能量，成為主序星。

Related Terms:

• 主序
• Star Formation
• Interstellar Medium
• 分子雲

Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher
The translation of this term and its definition is still awaiting approval

This is an automated transliteration of the simplified Chinese translation of this term

The OAE Multilingual Glossary is a project of the IAU Office of Astronomy for Education (OAE) in collaboration with the IAU Office of Astronomy Outreach (OAO). The terms and definitions were chosen, written and reviewed by a collective effort from the OAE, the OAE Centers and Nodes, the OAE National Astronomy Education Coordinators (NAECs) and other volunteers. You can find a full list of credits here. All glossary terms and their definitions are released under a Creative Commons CC BY-4.0 license and should be credited to "IAU OAE".