Glossary term: 星際介質
Description: 星際介質(ISM)是一個術語,用來描述星系中恆星系統之間的所有氣體和塵埃。我們的太陽系位於銀河系的銀盤中,這裡的大部分星際介質都是原子氫、原子氦和塵埃的混合物。
與行星大氣層相比,星際介質的密度非常低,其典型密度小於每立方釐米一個粒子,大約是地球大氣層密度的五千億億分之一。在整個銀河系中,ISM 的密度和溫度變化很大,分為幾個不同的組分。
銀盤中體積最大的星際介質組分是暖原子氣體和暖電離氣體,它們的溫度都在8000開爾文(K)左右,密度約為每立方釐米半個原子或離子。體積較小的星際介質組分以溫度約為40K的更冷、密度更大的原子氣體的形式存在。體積更小的星際介質組分是溫度更低(<20 K)、密度更大(每立方釐米高達一百萬個分子)的氫分子雲。其中一些分子雲會在自身引力的作用下坍縮,從而形成新的恆星。銀河系中的分子雲主要分布在旋臂中。銀盤周圍的氣體溫度極高(數百萬開爾文),密度極低。
恆星通過恆星風和超新星把氣體和塵埃注回星際介質。返回到星際介質的氣體和塵埃含有較多的重元素(金屬),因此隨著時間的推移,這些重元素在銀河系內的富集程度也在增加。星際介質中的氣體和塵埃是造成星際消光的主要原因。
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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 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
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