Glossary term: 星际介质
Description: 星际介质(ISM)是一个术语,用来描述星系中恒星系统之间的所有气体和尘埃。我们的太阳系位于银河系的银盘中,这里的大部分星际介质都是原子氢、原子氦和尘埃的混合物。
与行星大气层相比,星际介质的密度非常低,其典型密度小于每立方厘米一个粒子,大约是地球大气层密度的五千亿亿分之一。在整个银河系中,ISM 的密度和温度变化很大,分为几个不同的组分。
银盘中体积最大的星际介质组分是暖原子气体和暖电离气体,它们的温度都在8000开尔文(K)左右,密度约为每立方厘米半个原子或离子。体积较小的星际介质组分以温度约为40K的更冷、密度更大的原子气体的形式存在。体积更小的星际介质组分是温度更低(<20 K)、密度更大(每立方厘米高达一百万个分子)的氢分子云。其中一些分子云会在自身引力的作用下坍缩,从而形成新的恒星。银河系中的分子云主要分布在旋臂中。银盘周围的气体温度极高(数百万开尔文),密度极低。
恒星通过恒星风和超新星把气体和尘埃注回星际介质。返回到星际介质的气体和尘埃含有较多的重元素(金属),因此随着时间的推移,这些重元素在银河系内的富集程度也在增加。星际介质中的气体和尘埃是造成星际消光的主要原因。
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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
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".
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