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Glossary term: K 型星

Description: 光譜類型為 ”K“ 的恆星。天文學家通過光譜中氫原子譜線非常弱但鐵和錳原子譜線較強來識別 K 型星。它們的典型(有效)溫度大約在 3700 K 到 5200 K 之間。與其他恆星相比,它們在人眼中呈現橙白色,除非受到星際或大氣層紅化的影響。金牛座的畢宿五(即阿爾德巴朗)和雙子座的北河三(即波魯克斯)就是 K 型星。

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Term and definition status: The original definition of this term in English have been approved by a research astronomer and a teacher
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This is an automated transliteration of the simplified Chinese translation of this term

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Related Diagrams

一顆 K 型恒星的光譜

Caption: K 型恒星 2MASS J19554455+4754531 的光譜。波長在 400 納米到 700 納米之間的光譜綫的顔色大緻與人眼看到的該波長光綫的顔色一緻。波長低於 400 納米和高於 700 納米時,人眼幾乎看不到光,光譜綫分彆被染成藍色和紅色。 黑綫錶示恒星大氣中不同元素的原子和離子造成的光譜吸收綫。這些原子和離子會吸收特定波長的光,從而在光譜中形成尖銳的暗綫。這些綫條的強度取決於恒星大氣層的溫度。如果兩顆恒星的大氣層溫度不同,那麼由相同元素混閤而成的兩顆恒星的光譜中可能會齣現大相徑庭的綫條。K 型恒星的光譜主要由鐵、鈉和鈣等金屬原子構成。金屬原子的譜綫非常多,多到無法逐一標齣,以至於光譜看起來波瀾不驚、參差不齊。氫原子和鈣離子的譜綫比更熱的 G 型恒星要弱得多。
Credit: IAU OAE/SDSS/Niall Deacon

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