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X線天文衛星SuzakuおよびChandraを用いた小マゼラン星雲中の超新星残骸0103-72.6の観測的研究
http://hdl.handle.net/10458/1603
http://hdl.handle.net/10458/1603267e0c88-a04b-43b8-a68f-a7a1999e2971
名前 / ファイル | ライセンス | アクション |
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KJ00005015009.pdf (426.6 kB)
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Item type | 紀要論文 / Departmental Bulletin Paper(1) | |||||
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公開日 | 2008-11-11 | |||||
タイトル | ||||||
言語 | ja | |||||
タイトル | X線天文衛星SuzakuおよびChandraを用いた小マゼラン星雲中の超新星残骸0103-72.6の観測的研究 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | A study of the Supernova Remnant 0103-72.6 in the small Magellanic Cloud with Suzaku and Chandra X-ray Observatories | |||||
言語 | ||||||
言語 | jpn | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | SNR 0103-72.6, ejecta, ISM, Suzaku, Chandra | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
資源タイプ | departmental bulletin paper | |||||
その他(別言語等)のタイトル | ||||||
その他のタイトル | Xセン テンモン エイセイ Suzaku オヨビ Chandra オ モチイタ ショウマゼランセイウン チュウ ノ チョウシンセイ ザンガイ 0103-72.6 ノ カンソクテキ ケンキュウ | |||||
言語 | ja-Kana | |||||
著者 |
川井田, 英広
× 川井田, 英広× 木村, 結樹× 森, 浩二× Kawaida, Hidehiro× Kimura, Yuuki× Mori, Koji |
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抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | A supernova remnant (SNR) is the remains of the violent explosion of a star at the end of its life. High velocity shocks trigged by the explosion heat both the interstellar medium (ISM) and synthesized materials in progenitor star, called ejecta, to several million degree. Therefore, X-ray observations of SNRs allow us to investigate the constituents in ISM and ejecta. The SNR 0103-72.6 in the Small Magellanic Cloud (SMC), which is known to show clear sign of ejecta, has been observed with Suzaku and Chandra X-ray observatories. Suzaku and Chandra have better energy and spatial resolutions, respectively, compared to each other. Utilizing the respective advantages, we derived the elemental abundances of the ejecta of 0103 precisely. The abundances of light elements like O, Ne, Mg are highly elevated while those of heavy elements like Si and Fe are comparable to the SMC abundances, suggesting that 0103 is a remnant of a core-collapse explosion, not of a thermonuclear one. The relative abundance ratio indicates that the progenitor star had a 15-18 solar mass. | |||||
言語 | en | |||||
書誌情報 |
ja : 宮崎大学工学部紀要 en : Memoirs of Faculty of Engineering, University of Miyazaki 巻 37, p. 43-50, 発行日 2008-08-30 |
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出版者 | ||||||
言語 | ja | |||||
出版者 | 宮崎大学工学部 | |||||
出版者 | ||||||
言語 | en | |||||
出版者 | Faculty of Engineering, University of Miyazaki | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 05404924 | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA00732558 | |||||
著者版フラグ | ||||||
出版タイプ | VoR | |||||
出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 |