National Tsing Hua University Institutional Repository:AAS POSITION ON THE SPACE STATION
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    题名: AAS POSITION ON THE SPACE STATION
    作者: SHU, F.;NAJITA, J.;OSTRIKER, E.;WILKIN, F.;RUDEN, S.;LIZANO, S.
    教師: 徐遐生
    日期: 1994
    出版者: American Astronomical Society
    關聯: ASTROPHYSICAL JOURNAL, American Astronomical Society, Volume 429, Issue 2, Part 1, JUL 10 1994, Pages 781-796
    关键词: ASTRONOMICAL MODELS
    CENTRIFUGAL FORCE
    DISK GALAXIES
    MAGNETIC FIELDS
    MASS FLOW
    PROTOSTARS
    STELLAR MASS ACCRETION
    T TAURI STARS
    ANGULAR MOMENTUM
    NUMERICAL ANALYSIS
    STELLAR WINDS
    TERMINAL VELOCITY
    摘要: We propose a generalized model for stellar spin-down, disk accretion, and truncation, and the origin of winds, jets, and bipolar outflows from young stellar objects. We consider the steady state dynamics of accretion of matter from a viscous and imperfectly conducting disk onto a young star with a strong magnetic field. For an aligned stellar magnetosphere, shielding currents in the surface layers of the disk prevent stellar field lines from penetrating the disk everywhere except for a range of radii about omegaBAR = R(x), where the Keplerian angular speed of rotation OMEGA(x) equals the angular speed of the star OMEGA*. For the low disk accretion rates and high magnetic fields associated with typical T Tauri stars, R(x) exceeds the radius of the star R* by a factor of a few, and the inner disk is effectively truncated at a radius R(t) somewhat smaller than R(x). Where the closed field lines between R(t) and R(x) bow sufficiently inward, the accreting gas attaches itself to the field and is funneled dynamically down the effective potential (gravitational plus centrifugal) onto the star. Contrary to common belief, the accompanying magnetic torques associated with this accreting gas may transfer angular momentum mostly to the disk rather than to the star. Thus, the star can spin slowly as long as R(x) remains significantly greater than R*. Exterior to R(x) field lines threading the disk bow outward, which makes the gas off the midplane rotate at super-Keplerian velocities. This combination drives a magnetocentrifugal wind with a mass-loss rate M(w) equal to a definite fraction f of the disk accretion rate M(D). For high disk accretion rates, R(x) is forced down to the stellar surface, the star is spun to breakup, and the wind is generated in a manner identical to that proposed by Shu, Lizano, Ruden, & Najita in a previous communication to this journal. In two companion papers (II and III), we develop a detailed but idealized theory of the magnetocentrifugal acceleration process.
    相関连結: http://aas.org/
    URI: http://nthur.lib.nthu.edu.tw/dspace/handle/987654321/80965
    显示于类别:[ 徐遐生 (2002-2006)] 期刊論文
    [物理系] 期刊論文

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