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Orbital Modulation and a New Ephemeris of Cygnus X-3
https://jaxa.repo.nii.ac.jp/records/5039
https://jaxa.repo.nii.ac.jp/records/503949017caa-1e18-4286-93d0-6f190a7f035c
名前 / ファイル | ライセンス | アクション |
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64574107.pdf (499.9 kB)
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Item type | 会議発表論文 / Conference Paper(1) | |||||
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公開日 | 2015-03-26 | |||||
タイトル | ||||||
言語 | en | |||||
タイトル | Orbital Modulation and a New Ephemeris of Cygnus X-3 | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
言語 | en | |||||
主題Scheme | Other | |||||
主題 | Binaries: close - X-rays: binaries - stars: individual (Cygnus X-3) | |||||
資源タイプ | ||||||
資源タイプ識別子 | http://purl.org/coar/resource_type/c_5794 | |||||
資源タイプ | conference paper | |||||
著者 |
北本, 俊二
× 北本, 俊二× 長崎, 健太× 岸下, 徹一× Kitamoto, Shunji× Watanabe, Aya× Nagasaki, Kenta× Kishishita, Tetsuichi |
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著者所属 | ||||||
立教大学理学部物理学科 | ||||||
著者所属 | ||||||
立教大学理学部物理学科 | ||||||
著者所属 | ||||||
立教大学理学部物理学科 | ||||||
著者所属 | ||||||
宇宙航空研究開発機構宇宙科学研究本部 | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Rikkyo University | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Rikkyo University | ||||||
著者所属(英) | ||||||
en | ||||||
Department of Physics, Rikkyo University | ||||||
著者所属(英) | ||||||
en | ||||||
Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (ISAS)(JAXA) | ||||||
出版者 | ||||||
出版者 | 宇宙航空研究開発機構 | |||||
出版者(英) | ||||||
出版者 | Japan Aerospace Exploration Agency (JAXA) | |||||
書誌情報 |
宇宙航空研究開発機構特別資料: en : JAXA Special Publication: The Energetic Cosmos; from Suzaku to ASTRO-H 巻 JAXA-SP-09-008E, p. 288-289, 発行日 2010-02-26 |
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会議概要(会議名, 開催地, 会期, 主催者等)(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan | |||||
抄録(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We investigate an orbital X-ray modulation of the enigmatic X-ray binary, Cygnus X-3. It is a close binary system, composed of a Wolf-Rayet (WR) star and a compact star with a 4.8h orbital period. We determine a new precise orbital ephemeris and found that the orbital period is monotonically increasing with (1/2)P(dP/dt) = (5.62 +/- 0.09) x 10(sup -11) day, over more than three decades from 1970s. The obtained period derivative is explained by an intense stellar wind from the WR star with approximately 10(sup from -6 to -5) solar mass yr(sup -1). This mass loss rate is a reasonable value as a Wolf-Rayet star. This thick wind exposed to intense X-rays should be photo-ionized. Observed rich emission lines come from this photo-ionized plasma as well as some narrow radiative recombination continuums (RRCs). We investigate an orbital modulation of the emissions lines and the RRCs. We found that the emission lines show a large equivalent width around phase 0.0 (phase 0.0 means the X-ray intensity minimum phase). However, the RRCs show different modulation pattern from that of the emission lines. | |||||
内容記述(英) | ||||||
内容記述タイプ | Other | |||||
内容記述 | Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 1349-113X | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA11984031 | |||||
資料番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | 資料番号: AA0064574107 | |||||
レポート番号 | ||||||
内容記述タイプ | Other | |||||
内容記述 | レポート番号: JAXA-SP-09-008E |