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銀河団内ガス分布に対する新しいベータモデル
http://hdl.handle.net/10965/484
http://hdl.handle.net/10965/4841a2406db-49f7-46fc-a59b-54faff7302f2
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
AHSUSK_NSS_37_45.pdf (235.5 kB)
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| Item type | 紀要論文 / Departmental Bulletin Paper(1) | |||||
|---|---|---|---|---|---|---|
| 公開日 | 2017-09-30 | |||||
| タイトル | ||||||
| タイトル | 銀河団内ガス分布に対する新しいベータモデル | |||||
| 言語 | ja | |||||
| タイトル | ||||||
| タイトル | New β Model of Intracluster Gas Distribution | |||||
| 言語 | en | |||||
| 言語 | ||||||
| 言語 | eng | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | X線 | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | 銀河団 | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | 銀河団内ガス温度 | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | 密度分布 | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | ダークマター（暗黒物質） | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | X-rays | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | cluster of galaxies | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | intracluster gas temperature | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | density distribution | |||||
| キーワード | ||||||
| 言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | dark matter | |||||
| 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 | |||||
| 著者 |
三好, 蕃
× 三好, 蕃× 吉村, 将智× 田中, 伸広 |
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| 抄録 | ||||||
| 内容記述タイプ | Abstract | |||||
| 内容記述 | A new type of β model of intracluster gas distribution is established, which is well fitted to the observed X-ray surface brightness profile except for outermost region. It employs the exact King model of the self-gravitating system of collisionless particles instead of the widely used approximated analytical formula for the dark matter distribution. The small difference between the modelled and the observed X-ray surface brightness profiles would disappear if the infall of matter from the intercluster space is taken into account. The number of parameters of our model is the same as for the isothermal β model, but the agreement between our model and data points is satisfactory even when the fitting with the isothermal β model remaines a large central excess. In addition, the enhanced central mass concentration in our model is high enough to resolve the discrepancy between the X-ray and the lensing measurements of cluster mass. These facts suggest that most of the central excess might be no more than a ghost embossed by an inadequate fitting. Therefore the central excess would not necessarily be linked to the existence of cooling flow. It is also shown that the obtained values of β(our model)∼0.5support the theory of non-gravitational intracluster gas heatings comparable to those reached through gravitational collapse. On the other hand, the value of β∼0.6obtained for the isothermal β model is explained as showing the scarcity of matter in the space surrounding each cluster, brobably due to the infall of matter towards it over a long time. | |||||
| 書誌情報 |
京都産業大学論集. 自然科学系列 巻 37, p. 45-58, 発行日 2008-03 |
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| 出版者 | ||||||
| 出版者 | 京都産業大学 | |||||
| ISSN | ||||||
| 収録物識別子タイプ | PISSN | |||||
| 収録物識別子 | 1348-3323 | |||||
| 書誌レコードID | ||||||
| 収録物識別子タイプ | NCID | |||||
| 収録物識別子 | AA11923897 | |||||
| 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 | |||||
