Description: 恆星的冕是圍繞恆星大氣層的極熱、低密度的等離子體區域，可以在宇宙空間中延伸數百萬千米。每一顆具有相當強磁場的恆星都會有一個冕，這種磁場源於恆星內部帶電物質運動時產生的發電機效應。在日全食時，我們可以用肉眼觀測到一個形狀不規則的白色區域，環繞著被遮掩的太陽圓面，這就是太陽的冕（即“日冕”）。一般來說，恆星冕的形狀是由恆星的磁場及其上部區域氣體的外壓決定的。恆星冕的溫度非常高：例如，日冕的溫度超過一百萬開爾文，比太陽表面的溫度高得多。將日冕加熱到這一溫度的機制是目前正在研究的課題，但似乎很清楚的是，貫穿日冕的磁場發揮了重要作用。日冕形狀變化的時間尺度在幾秒到幾個月之間，主要是太陽活動所引發的，如耀斑將等離子體噴射到日冕，或日冕物質拋射釋放大量帶電粒子。日冕還會隨著所謂的太陽週期（太陽磁場強度和方向的週期性變化，週期近 11 年）的變化而在數年的時間尺度上發生變化。預計其他恆星的冕也會發生類似的變化。

Related Terms:

• 色球
• 太陽耀斑
• 日珥
• 太陽風
• 恆星結構

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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