高偏振星

Multi tool use
高偏振星(Polar)或武仙座AM型變星(AM Herculis Star)是有強磁場的雙星系統形成的激變變星。
大部分的激變變星,都有一顆被白矮星的引力剝離外殼的主序星做為伴星,並因而形成吸積盤。在偏極化的系統中,白矮星的磁場對吸積盤的形成是太強了,因此落向白矮星的氣體只能跟隨著白矮星的偶極子磁場線形成吸積流。
典型的磁場強度在1,000萬至8,000萬高斯(1,000至8,000T)。大熊座AN是已知磁場最強的激變變星,磁場強度高達2億3,000萬高斯(23KT)。
高偏振的名稱來自於磁場造成光線的線性偏極和圓偏極。極化現象對偏極的研究是很重要的,可以透過對極化的研究了解雙星的幾何結構。
相關條目
參考資料
Coel Hellier. Cataclysmic Variable Stars: How and Why They Vary. Springer Praxis. 2001. ISBN 1-85233-211-5.
白矮星
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形成 |
- 錢德拉塞卡極限
- PG 1159星
- 恆星演化
- 赫羅圖
- 米拉變星
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宿命 |
- 黑矮星
Ia超新星
中子星
恆星黑洞
致密星
- 臨終氦星
- B型次矮星
- 氦行星
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双星系统 |
新星
- 矮新星
- 共生變星
激變變星
X射線聯星
聯星脈衝星
- 氦閃
- 碳引爆
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屬性 |
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相關的 |
行星狀星雲
大质量重子天体强关联星团(RAMBOs)
- 白矮星光度函數
- 白矮星、中子星和超新星年表
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著名的 |
- 范馬南星
- 天狼星B
- 南河三B
- 波江座40 B
- BPM 37093
- HL金牛座76
- 蛇夫座RS
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