Accretion-Disk Corona Advected by External Radiation Drag I.

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We examined an accretion-disk corona (beta-corona) which is dynamically driven via the radiation drag exerted by a central luminous source and the accretion disk, itself. We adopted the standard alpha-disk as the disk model. We considered a geometrically thin and optically thin corona and ignored any motion such as wind. When the central source is sufficiently luminous, the specific angular momentum of the corona gas is lost by the radiation drag of the radiation field produced by the central source. As a result, the rotation velocity of the corona gas becomes smaller than a Keplerian one, and the corona gas is advected inward on a dynamical timescale. This new picture concerning the accretion-disk corona - a dynamical disk corona - is a rather universal one. When the accretion disk is luminous, on the other hand, the corona gas tends to corotate with the underlying disk by radiation drag of the radiation field produced by the alpha-disk. As a result, the advection of the corona gas is suppressed (this is the case of the traditional picture of a stationary disk corona). In addition, the emission-line profiles expected from these advected disk corona can be calculated for a wide variety of parameters. The line profiles are generally double peaked. The separation of two peaks depends on the brightness of the central source as well as the size of the emitting regions. When the central source is brighter, the separation of two peaks becomes smaller.

収録刊行物

  • PASJ : publications of the Astronomical Society of Japan

    PASJ : publications of the Astronomical Society of Japan 48(6), 841-848, 1996-12-01

    Astronomical Society of Japan

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各種コード

  • NII論文ID(NAID)
    10002596637
  • NII書誌ID(NCID)
    AA1082896X
  • 本文言語コード
    ENG
  • 資料種別
    ART
  • ISSN
    00046264
  • NDL 記事登録ID
    4109455
  • NDL 雑誌分類
    ZM33(科学技術--宇宙科学)
  • NDL 請求記号
    Z53-A296
  • データ提供元
    CJP書誌  NDL  IR 
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