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  1. 010 学術雑誌論文
  2. 池内, 了 / IKEUCHI, Satoru

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/3515
ebed975d-9d29-4e86-8b0b-1e11343fa6be
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nph-iarticle_query15.pdf nph-iarticle_query15 (585.5 kB)
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Item type 学術雑誌論文 / Journal Article(1)
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

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LI, Fan

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IKEUCHI, Satoru

× IKEUCHI, Satoru

IKEUCHI, Satoru

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著者別名 池内, 了

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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
出版者
出版者 The American Astronomical Society
ISSN
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
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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
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