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The circumstellar gas of helium-rich stars will be trapped in the outer region of stellar magnetosphere where the centrifugal force dominates. Only in rapidly rotating stars, the outer region can contain the gas much enough to emit the observed Hα emission energy flux. As the circumstellar gas corotates with the star, the Hα emission profile becomes very broad and so the emission will appear in the wing of Hα absorption line which originates in the photosphere of star.
紀要類(bulletin)
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収録刊行物
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- The science reports of the Tohoku University. Ser. 8, Physics and astronomy
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The science reports of the Tohoku University. Ser. 8, Physics and astronomy 2 (3), 130-142, 1981-12-05
Faculty of Science, Tohoku University
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詳細情報 詳細情報について
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- CRID
- 1050282677707831936
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- NII書誌ID
- AA00441828
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- ISSN
- 03885607
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- HANDLE
- 10097/25480
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- 本文言語コード
- en
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- 資料種別
- departmental bulletin paper
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- データソース種別
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- IRDB