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Formation of a giant galactic gaseous halo: Metal absorption lines and high-velocity clouds
https://ir.soken.ac.jp/records/3515
https://ir.soken.ac.jp/records/3515ebed975d-9d29-4e86-8b0b-1e11343fa6be
| 名前 / ファイル | ライセンス | アクション |
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nph-iarticle_query15 (585.5 kB)
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| Item type | 学術雑誌論文 / Journal Article(1) | |||||||||
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| 公開日 | 2013-04-25 | |||||||||
| タイトル | ||||||||||
| タイトル | Formation of a giant galactic gaseous halo: Metal absorption lines and high-velocity clouds | |||||||||
| タイトル | ||||||||||
| タイトル | Formation of a giant galactic gaseous halo: Metal absorption lines and high-velocity clouds | |||||||||
| 言語 | en | |||||||||
| 言語 | ||||||||||
| 言語 | eng | |||||||||
| 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 | journal article | |||||||||
| 著者 |
LI, Fan
× LI, Fan
× IKEUCHI, Satoru
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| 著者別名 |
池内, 了
× 池内, 了
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| 抄録 | ||||||||||
| 内容記述タイプ | Abstract | |||||||||
| 内容記述 | A Galactic gaseous halo formed through the interstellar disk-halo connection is simulated by means of a two-dimensional axisymmetric hydrodynamic code based upon the chimney model of the interstellar medium - a new version of a galactic fountain. Galactic rotation, heating processes by diffuse UV flux, and radiative cooling processes are taken into account. The resulting gaseous halo can be classified as belonging to one of three categories: wind-type halos, bound-type halos and cooled-type halos. The abundance of each ion of H, He, and heavy elements is calculated according to the hydrodynamic and thermal state of the halo gas. In this way, we try to reproduce the column densities of C IV, N V, O VI, and Si IV in the observed absorption lines of halo stars. Assuming that the radiatively cooled halo gas condenses into clouds due to thermal instabilities, we calculate the distribution and ballistic motions of the clouds in the Galactic gravitational field. These correspond to the high- and intermediate-velocity clouds observed at high Galactic latitudes. We find that a cooled-type halo with gas temperature between 5 × 10 5 and 10 6 K and density between 10 -3 and 10 -2 cm -3 at the disk-halo interface can reproduce the observational facts about our Galaxy. Supposing that the metal absorption-line systems of QSOs arise from the halos of intervening galaxies formed by similar processes, we calculate features of the Ca II, Mg II, C IV, and Si IV absorption lines in various stages of the galaxies' evolution. We conclude that C IV systems greater than 50 kpc correspond to the wind-type halo. Contrarily, Mg II and Ca II systems can be detected in a very restricted region (≤20 kpc). | |||||||||
| 書誌情報 |
Astrophysical Journal, Part 1 en : Astrophysical Journal, Part 1 巻 390, 号 2, p. 405-422, 発行日 1992-05 |
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| 出版者 | ||||||||||
| 出版者 | The American Astronomical Society | |||||||||
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| 収録物識別子タイプ | ISSN | |||||||||
| 収録物識別子 | 20418205 | |||||||||
| DOI | ||||||||||
| 関連タイプ | isIdenticalTo | |||||||||
| 識別子タイプ | DOI | |||||||||
| 関連識別子 | http://doi.org/10.1086/171291 | |||||||||
| 関連名称 | 10.1086/171291 | |||||||||
| 権利 | ||||||||||
| 権利情報 | © 1992. The American Astronomical Society. | |||||||||
| 関連サイト | ||||||||||
| 識別子タイプ | URI | |||||||||
| 関連識別子 | http://aas.org/publications/aas-copyright-policy | |||||||||
| 関連名称 | Copyright | |||||||||
| フォーマット | ||||||||||
| 内容記述タイプ | Other | |||||||||
| 内容記述 | application/pdf | |||||||||
| 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 | |||||||||
